From 38086572c83a3882961ef5b14e66e7a01de54ddf Mon Sep 17 00:00:00 2001 From: houlinfeng Date: Fri, 20 Sep 2024 16:02:07 +0800 Subject: [PATCH] feat: mineru web and web_api --- .gitignore | 3 +- projects/web/README.md | 2 +- projects/web/package.json | 2 + projects/web/src/pages/home.tsx | 6 +-- projects/web_api/README.md | 43 ++++++++++------- projects/web_api/mineru-web接口文档.html | 2 +- projects/web_api/requirements.txt | 13 ++++++ projects/web_api/web_api/api/__init__.py | 4 +- .../web_api/web_api/api/analysis/__init__.py | 4 +- .../web_api/api/analysis/analysis_view.py | 9 ++-- .../web_api/api/analysis/markdown_view.py | 44 ++++++++++++++++++ projects/web_api/web_api/api/extentions.py | 1 + .../web_api/web_api/api/react_app/__init__.py | 11 +++++ .../web_api/api/react_app/react_app_view.py | 11 +++++ projects/web_api/web_api/config/config.yaml | 2 + projects/web_api/web_api/config/mineru_web.db | Bin 557056 -> 12288 bytes 16 files changed, 128 insertions(+), 29 deletions(-) create mode 100644 projects/web_api/requirements.txt create mode 100644 projects/web_api/web_api/api/analysis/markdown_view.py create mode 100644 projects/web_api/web_api/api/react_app/__init__.py create mode 100644 projects/web_api/web_api/api/react_app/react_app_view.py diff --git a/.gitignore b/.gitignore index c0a2706a..f7f427f3 100644 --- a/.gitignore +++ b/.gitignore @@ -38,4 +38,5 @@ source.dev.env tmp -projects/web/node_modules \ No newline at end of file +projects/web/node_modules +projects/web/dist diff --git a/projects/web/README.md b/projects/web/README.md index f39bbe28..cc592819 100644 --- a/projects/web/README.md +++ b/projects/web/README.md @@ -8,5 +8,5 @@ npm install -g pnpm 3. build ``` 1.pnpm run build -2.npm run buil +2.npm run build ``` \ No newline at end of file diff --git a/projects/web/package.json b/projects/web/package.json index 2b135258..c2044ac9 100644 --- a/projects/web/package.json +++ b/projects/web/package.json @@ -22,9 +22,11 @@ "ahooks": "^3.8.1", "antd": "^5.20.3", "axios": "^1.7.5", + "canvas": "^2.11.2", "classnames": "^2.5.1", "js-cookie": "^3.0.5", "lodash": "^4.17.21", + "path2d": "^0.2.1", "qs": "^6.13.0", "react": "^18.3.1", "react-copy-to-clipboard": "^5.1.0", diff --git a/projects/web/src/pages/home.tsx b/projects/web/src/pages/home.tsx index 5ebd1c49..c162e902 100644 --- a/projects/web/src/pages/home.tsx +++ b/projects/web/src/pages/home.tsx @@ -3,7 +3,7 @@ import ErrorBoundary from "@/components/error-boundary"; import styles from "./home.module.scss"; import { SlotID, Path } from "@/constant/route"; -import { BrowserRouter, Routes, Route, Outlet } from "react-router-dom"; +import { HashRouter, Routes, Route, Outlet } from "react-router-dom"; import { ExtractorSide } from "./extract-side"; import { LanguageProvider } from "@/context/language-provider"; import PDFUpload from "@/pages/extract/components/pdf-upload"; @@ -70,9 +70,9 @@ export function Home() { return ( - + - + ); diff --git a/projects/web_api/README.md b/projects/web_api/README.md index 5580d72c..849654dd 100644 --- a/projects/web_api/README.md +++ b/projects/web_api/README.md @@ -1,34 +1,43 @@ -## 安装 +## Mineru 本地API服务 MinerU -```bash -# mineru已安装则跳过此步骤 - -git clone https://github.com/opendatalab/MinerU.git -cd MinerU - -conda create -n MinerU python=3.10 -conda activate MinerU -pip install .[full] --extra-index-url https://wheels.myhloli.com +``` +# 服务依赖mineru，请先确保mineru已安装 ``` -第三方软件 +1. 打包前端界面 ```bash +# 先进入前端目录 +cd projects/web +# 打包前端项目 +npm install -g yarn +yarn install +yarn build +``` + +2. 安装服务依赖 + +```bash +# 先进入后端目录 cd projects/web_api -pip install poetry -portey install +# 安装依赖 +pip3 install -r requirements.txt -i https://pypi.tuna.tsinghua.edu.cn/simple ``` -启动服务 +3. 启动服务 ```bash -cd web_api -python app.py +# 进入程序目录 +cd projects/web_api/web_api +# 启动服务 +python3 app.py +# 在浏览器访问启动的地址即可访问界面 ``` -接口文档 +ps：接口文档 + ``` 在浏览器打开 mineru-web接口文档.html ``` diff --git a/projects/web_api/mineru-web接口文档.html b/projects/web_api/mineru-web接口文档.html index 0c5fddbb..93f31f60 100644 --- a/projects/web_api/mineru-web接口文档.html +++ b/projects/web_api/mineru-web接口文档.html @@ -44,7 +44,7 @@ window.onload = function() { // Begin Swagger UI call region const ui = SwaggerUIBundle({ - spec: 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This mechanism causes the magnetic field to become increasingly parallel to the","score":1,"type":"text"}]},{"bbox":[59,408.172119140625,535,418.97662353515625],"spans":[{"bbox":[59.5279541015625,408.172119140625,535.7513427734375,418.97662353515625],"content":"dense layer, and the development of a shear flow around the latter. Furthermore, the bending-mode perturbations on the dense layer","score":1,"type":"text"}]},{"bbox":[59,418.1351318359375,535,428.93963623046875],"spans":[{"bbox":[59.5279541015625,418.1351318359375,535.7510375976562,428.93963623046875],"content":"are amplified by the non-linear thin-shell instability (NTSI), stretching the density structures formed by the thermal instability, and","score":1,"type":"text"}]},{"bbox":[59,428.09814453125,535,438.90264892578125],"spans":[{"bbox":[59.5279541015625,428.09814453125,355.9569396972656,438.90264892578125],"content":"rendering them parallel to the bent field lines. 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We also find that the upstream superalfvénic regime transitions to a transalfvénic regime between the shock","score":1,"type":"text"}]},{"bbox":[59,457.98516845703125,535,468.7896728515625],"spans":[{"bbox":[59.5279541015625,457.98516845703125,535.7510375976562,468.7896728515625],"content":"and the condensation front, and then to a subalfvénic regime inside the condensations. Finally, in two-dimensional simulations with a","score":1,"type":"text"}]},{"bbox":[59,467.94818115234375,524.3818969726562,478.752685546875],"spans":[{"bbox":[59.5279541015625,467.94818115234375,524.3818969726562,478.752685546875],"content":"curved collision front, the presence of the magnetic field inhibits the generation of turbulence by the shear around the dense layer.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[59,477.91119384765625,535,498.6777038574219],"lines":[{"bbox":[59,477.91119384765625,535,488.7156982421875],"spans":[{"bbox":[59.5279541015625,478.0784912109375,108.1572265625,488.623779296875],"content":"Conclusions.","score":1,"type":"text"},{"bbox":[108.1572265625,477.91119384765625,535.7467651367188,488.7156982421875],"content":" Our results provide a feasible physical mechanism for the observed transition from parallel to perpendicular relative","score":1,"type":"text"}]},{"bbox":[59,487.8731994628906,529,498.6777038574219],"spans":[{"bbox":[59.5279541015625,487.8731994628906,528.9368286132812,498.6777038574219],"content":"orientation of the magnetic field and the density structures as the density structures become increasingly dominated by self-gravity.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[59,503.8141784667969,420.0631103515625,514.7141723632812],"lines":[{"bbox":[59,503.8141784667969,420.0631103515625,514.7141723632812],"spans":[{"bbox":[59.5279541015625,504.0155334472656,104.37522888183594,514.7141723632812],"content":"Key words.","score":1,"type":"text"},{"bbox":[104.37522888183594,503.8141784667969,420.0631103515625,514.61865234375],"content":" Magnetic fields – ISM: clouds –ISM: magnetic fields – ISM: kinematics and dynamics","score":1,"type":"text"}]}],"type":"text"},{"bbox":[38,537,109,550],"lines":[{"bbox":[36.849952697753906,538.0780639648438,109.05316162109375,551.0947875976562],"spans":[{"bbox":[36.849952697753906,538.0780639648438,109.05316162109375,551.0947875976562],"content":"1. 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Magnetic fields are thought to be an important ingre-","score":1,"type":"text"}]},{"bbox":[37,606.5046997070312,291,618.5096435546875],"spans":[{"bbox":[36.849952697753906,606.5046997070312,291.97216796875,618.5096435546875],"content":"dient in the dynamics of the ISM, providing a possible support","score":1,"type":"text"}]},{"bbox":[37,617.4636840820312,291,629.4686279296875],"spans":[{"bbox":[36.849952697753906,617.4636840820312,291.97222900390625,629.4686279296875],"content":"mechanism against gravitational collapse, and guiding the gas","score":1,"type":"text"}]},{"bbox":[37,628.4226684570312,291,640.4276123046875],"spans":[{"bbox":[36.849952697753906,628.4226684570312,291.9721984863281,640.4276123046875],"content":"flow in the surroundings of filamentary structures, among many","score":1,"type":"text"}]},{"bbox":[37,639.3817138671875,291,651.3866577148438],"spans":[{"bbox":[36.849952697753906,639.3817138671875,65.88097381591797,651.3866577148438],"content":"other e","score":1,"type":"text"},{"bbox":[65.87995147705078,641.0350341796875,71.85751342773438,650.9976196289062],"content":"ff","score":1,"type":"text"},{"bbox":[71.85694885253906,639.3817138671875,291.9705810546875,651.3866577148438],"content":"ects. 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For example, Clark et al.","score":1,"type":"text"}]},{"bbox":[37,672.2586669921875,291,684.2636108398438],"spans":[{"bbox":[36.84994888305664,672.2586669921875,291.97222900390625,684.2636108398438],"content":"(2015) found that the plane of the sky magnetic field, measured","score":1,"type":"text"}]},{"bbox":[37,683.2166748046875,291,695.2216186523438],"spans":[{"bbox":[36.84994888305664,683.2166748046875,291.9721984863281,695.2216186523438],"content":"using polarized thermal dust emission, is aligned with atomic","score":1,"type":"text"}]},{"bbox":[37,694.1756591796875,291,706.1806030273438],"spans":[{"bbox":[36.84994888305664,694.1756591796875,291.97222900390625,706.1806030273438],"content":"hydrogen structures detected with HI emission and Clark et al.","score":1,"type":"text"}]},{"bbox":[37,705.1346435546875,291,717.1395874023438],"spans":[{"bbox":[36.84994888305664,705.1346435546875,234.73712158203125,717.1395874023438],"content":"(2014) also observed a similar alignment in HI","score":1,"type":"text"},{"bbox":[234.73712158203125,705.1346435546875,260.9491882324219,717.0299682617188],"content":" fibers","score":1,"type":"text"},{"bbox":[260.9489440917969,705.1346435546875,291.97247314453125,717.1395874023438],"content":", which","score":1,"type":"text"}]},{"bbox":[37,716.0936889648438,291,728.0986328125],"spans":[{"bbox":[36.849945068359375,716.0936889648438,291.9721984863281,728.0986328125],"content":"are thin long dense structures identified in HI emission using","score":1,"type":"text"}]},{"bbox":[37,727.0526733398438,291,739.0576171875],"spans":[{"bbox":[36.849945068359375,727.0526733398438,291.9721374511719,739.0576171875],"content":"the Rolling Hough transform. 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These intervals comprise the densities of the post-shock","score":1,"type":"text"}]},{"bbox":[35,406,291,418.8902587890625],"spans":[{"bbox":[36.84999084472656,406.88531494140625,83.08641052246094,418.8902587890625],"content":"warm neutr","score":1,"type":"text"},{"bbox":[129,406,202,417],"content":"\\bar{(n\\in[3,10]\\ \\mathrm{cm}^{-3})}","score":0.9,"type":"inline_equation"},{"bbox":[200.50498962402344,406.88531494140625,291.9715881347656,418.8902587890625],"content":"), the low-density cold","score":1,"type":"text"}]},{"bbox":[35,417,291,429.8492431640625],"spans":[{"bbox":[36.84999084472656,417.84429931640625,81.05404663085938,429.8492431640625],"content":"neutral gas","score":1,"type":"text"},{"bbox":[83,417,183,429],"content":"(n\\,\\in\\,[10,3\\times10^{1}]\\;\\mathrm{cm}^{-3})","score":0.87,"type":"inline_equation"},{"bbox":[182.13999938964844,417.84429931640625,291.9676818847656,429.8492431640625],"content":"), the medium-density cold","score":1,"type":"text"}]},{"bbox":[82,428.80328369140625,291,440.8082275390625],"spans":[{"bbox":[82,429,178,439],"content":"(n\\in[3{\\times}10^{1},10^{2}]\\,\\mathrm{cm}^{-3})","score":0.84,"type":"inline_equation"},{"bbox":[175.00701904296875,428.80328369140625,291.9678955078125,440.8082275390625],"content":"), the high-density neutral gas","score":1,"type":"text"}]},{"bbox":[35,439,291,458.3724060058594],"spans":[{"bbox":[36,439,133,451],"content":"(n\\in[10^{2},3\\times10^{2}]\\,\\mathrm{cm}^{-3})","score":0.86,"type":"inline_equation"},{"bbox":[45.149322509765625,440.340087890625,53.25697708129883,458.3724060058594],"content":" ∈","score":1,"type":"text"},{"bbox":[154.26364135742188,439.76226806640625,291.9666442871094,451.7672119140625],"content":" the density range of the central re-","score":1,"type":"text"}]},{"bbox":[35,450.72125244140625,291,469.3313903808594],"spans":[{"bbox":[36.85002136230469,450.72125244140625,59.98318099975586,462.7261962890625],"content":"gion (","score":1,"type":"text"},{"bbox":[56,451,152,462],"content":"(n\\in[3{\\times}10^{2},10^{3}]\\,\\mathrm{cm}^{-3})","score":0.87,"type":"inline_equation"},{"bbox":[64.96131896972656,451.299072265625,73.0689697265625,469.3313903808594],"content":" ∈","score":1,"type":"text"},{"bbox":[84.89701843261719,451.299072265625,91.23323059082031,469.3313903808594],"content":"×","score":1,"type":"text"},{"bbox":[150.0530242919922,450.72125244140625,167.36802673339844,462.7261962890625],"content":"). 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We keep this convention to compare to the three-","score":1,"type":"text"}]},{"bbox":[35,505.51617431640625,291,517.5211181640625],"spans":[{"bbox":[36.85002899169922,505.51617431640625,291.9722900390625,517.5211181640625],"content":"dimensional HRO diagram presented in Soler et al. (2013). We","score":1,"type":"text"}]},{"bbox":[35,516.4741821289062,291,528.4791259765625],"spans":[{"bbox":[36.85002899169922,516.4741821289062,246.95132446289062,528.4791259765625],"content":"can see that the HRO for all density intervals peaks at ","score":1,"type":"text"},{"bbox":[246,517,289,528],"content":"\\cos(\\phi)=0","score":0.91,"type":"inline_equation"},{"bbox":[289.19830322265625,516.4741821289062,291.9678955078125,528.4791259765625],"content":";","score":1,"type":"text"}]},{"bbox":[35,527.4331665039062,291,539.4381103515625],"spans":[{"bbox":[36.850006103515625,527.4331665039062,291.9723205566406,539.4381103515625],"content":"in other words, the magnetic field tends to be parallel to the den-","score":1,"type":"text"}]},{"bbox":[35,538.3921508789062,270.9013671875,550.3970947265625],"spans":[{"bbox":[36.850006103515625,538.3921508789062,270.9013671875,550.3970947265625],"content":"sity structures throughout the density range we investigate.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[35,549.7291259765625,291,572.693115234375],"lines":[{"bbox":[51,549.7291259765625,291,561.7340698242188],"spans":[{"bbox":[51.79400634765625,549.7291259765625,291.9723205566406,561.7340698242188],"content":"In order to quantify the HRO, Soler et al. 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In that work, the authors sample density values","score":1,"type":"text"}]},{"bbox":[302,178.4664306640625,558,194.08738708496094],"spans":[{"bbox":[301,181,440,193],"content":"n\\ \\stackrel{\\cdot}{\\in}\\ [1.6\\times10^{2},3.16\\times10^{6}]\\ \\ \\mathrm{cm}^{3}","score":0.68,"type":"inline_equation"},{"bbox":[438.8199157714844,178.4664306640625,443.08001708984375,194.08738708496094],"content":" ","score":1,"type":"text"},{"bbox":[443.08001708984375,182.08245849609375,558.427001953125,194.08738708496094],"content":"in isothermal simulations of","score":1,"type":"text"}]},{"bbox":[302,193.04144287109375,558,205.04637145996094],"spans":[{"bbox":[303.3070068359375,193.04144287109375,558.4293212890625,205.04637145996094],"content":"cold molecular gas. In contrast, since we are interested in under-","score":1,"type":"text"}]},{"bbox":[302,204.00042724609375,558,216.00535583496094],"spans":[{"bbox":[303.3070068359375,204.00042724609375,558.42919921875,216.00535583496094],"content":"standing how this correlation arises as the cloud is assembled,","score":1,"type":"text"}]},{"bbox":[302,214.95941162109375,558,226.96434020996094],"spans":[{"bbox":[303.3070068359375,214.95941162109375,558.4292602539062,226.96434020996094],"content":"our simulation starts with warm atomic gas leading to density","score":1,"type":"text"}]},{"bbox":[302,225,558,237.92332458496094],"spans":[{"bbox":[303.3070068359375,225.91839599609375,362.1659851074219,237.92332458496094],"content":"structures with","score":1,"type":"text"},{"bbox":[363,225,483,237],"content":"n\\in[6\\times10^{-1},2.2\\times10^{3}]~\\bar{\\mathrm{cm}}^{3}.","score":0.73,"type":"inline_equation"},{"bbox":[483.9856262207031,225.91839599609375,558.4263305664062,237.92332458496094],"content":" Therefore, the ob-","score":1,"type":"text"}]},{"bbox":[302,236.87738037109375,558,248.88230895996094],"spans":[{"bbox":[303.30694580078125,236.87738037109375,558.42919921875,248.88230895996094],"content":"tained HRO shape parameter in Figure 3 complements the one","score":1,"type":"text"}]},{"bbox":[302,247.83636474609375,558,259.84130859375],"spans":[{"bbox":[303.30694580078125,247.83636474609375,558.4290161132812,259.84130859375],"content":"obtained by Soler et al. 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(2013).","score":1,"type":"text"}]}],"type":"text"},{"bbox":[302,337.99127197265625,558,426.7081298828125],"lines":[{"bbox":[318,337.99127197265625,558,349.9962158203125],"spans":[{"bbox":[318.2509460449219,337.99127197265625,558.4293212890625,349.9962158203125],"content":"In Figure 4, we show the density structures between the four","score":1,"type":"text"}]},{"bbox":[302,348.95025634765625,558,360.9552001953125],"spans":[{"bbox":[303.30694580078125,348.95025634765625,558.4291381835938,360.9552001953125],"content":"highest density intervals used to obtain the HRO and shape pa-","score":1,"type":"text"}]},{"bbox":[302,359.90924072265625,558,371.9141845703125],"spans":[{"bbox":[303.30694580078125,359.90924072265625,558.4292602539062,371.9141845703125],"content":"rameter of Figure 3. It can be seen from this figure that the mag-","score":1,"type":"text"}]},{"bbox":[302,370.86822509765625,558,382.8731689453125],"spans":[{"bbox":[303.30694580078125,370.86822509765625,558.4290771484375,382.8731689453125],"content":"netic field (black arrows) tends to be parallel to the density struc-","score":1,"type":"text"}]},{"bbox":[302,381.82623291015625,558,393.8311767578125],"spans":[{"bbox":[303.30694580078125,381.82623291015625,558.4292602539062,393.8311767578125],"content":"tures for the four density intervals. However, for the highest den-","score":1,"type":"text"}]},{"bbox":[302,392.78521728515625,558,404.7901611328125],"spans":[{"bbox":[303.30694580078125,392.78521728515625,558.42919921875,404.7901611328125],"content":"sity interval, the magnetic field does not follow this general trend","score":1,"type":"text"}]},{"bbox":[302,403.74420166015625,558,415.7491455078125],"spans":[{"bbox":[303.30694580078125,403.74420166015625,558.4291381835938,415.7491455078125],"content":"in some regions, leading to the observed change in the shape pa-","score":1,"type":"text"}]},{"bbox":[302,414.70318603515625,335.6754455566406,426.7081298828125],"spans":[{"bbox":[303.30694580078125,414.70318603515625,335.6754455566406,426.7081298828125],"content":"rameter.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[303,456,453,468],"lines":[{"bbox":[303.30694580078125,456.5015869140625,453.48583984375,469.51824951171875],"spans":[{"bbox":[303.30694580078125,456.5015869140625,453.48583984375,469.51824951171875],"content":"4. Magnetic field line evolution","score":1,"type":"text"}]}],"type":"title"},{"bbox":[302,476.9701843261719,558,576.6460571289062],"lines":[{"bbox":[302,476.9701843261719,558,488.9751281738281],"spans":[{"bbox":[303.30694580078125,476.9701843261719,558.4291381835938,488.9751281738281],"content":"To understand the alignment of the magnetic field with CACs","score":1,"type":"text"}]},{"bbox":[302,487.92919921875,558,499.93414306640625],"spans":[{"bbox":[303.30694580078125,487.92919921875,558.42919921875,499.93414306640625],"content":"shown in the previous section, we followed the evolution of the","score":1,"type":"text"}]},{"bbox":[302,498.88720703125,558,510.89215087890625],"spans":[{"bbox":[303.30694580078125,498.88720703125,558.42919921875,510.89215087890625],"content":"magnetic field lines. The resulting configuration of the three-","score":1,"type":"text"}]},{"bbox":[302,509.84619140625,558,521.8511352539062],"spans":[{"bbox":[303.30694580078125,509.84619140625,558.42919921875,521.8511352539062],"content":"dimensional density structures and magnetic field lines of Re-","score":1,"type":"text"}]},{"bbox":[302,520.80517578125,558,532.8101196289062],"spans":[{"bbox":[303.30694580078125,520.80517578125,558.42919921875,532.8101196289062],"content":"gion R1 after 5 Myr of evolution is shown in Figure 2, where","score":1,"type":"text"}]},{"bbox":[302,531.76416015625,558,543.7691040039062],"spans":[{"bbox":[303.30694580078125,531.76416015625,558.4293823242188,543.7691040039062],"content":"we can see the shock fronts at each side of the central condensa-","score":1,"type":"text"}]},{"bbox":[302,542.72314453125,558,554.7280883789062],"spans":[{"bbox":[303.30694580078125,542.72314453125,558.4290161132812,554.7280883789062],"content":"tion region. The magnetic field lines start bending at these shock","score":1,"type":"text"}]},{"bbox":[302,553.68212890625,558,565.6870727539062],"spans":[{"bbox":[303.30694580078125,553.68212890625,558.42919921875,565.6870727539062],"content":"fronts along their way from the center of the computational do-","score":1,"type":"text"}]},{"bbox":[302,564.64111328125,326,576.6460571289062],"spans":[{"bbox":[303.30694580078125,564.64111328125,325.7228088378906,576.6460571289062],"content":"main.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[302,578.0841064453125,558,633.924072265625],"lines":[{"bbox":[318,578.0841064453125,558,590.0890502929688],"spans":[{"bbox":[318.2509460449219,578.0841064453125,558.4293823242188,590.0890502929688],"content":"As can be seen in the provided animation (Fig. 2), the mag-","score":1,"type":"text"}]},{"bbox":[302,589.0430908203125,558,601.0480346679688],"spans":[{"bbox":[303.30694580078125,589.0430908203125,558.4290771484375,601.0480346679688],"content":"netic field lines change their direction from being nearly parallel","score":1,"type":"text"}]},{"bbox":[302,600.0020751953125,558,612.0070190429688],"spans":[{"bbox":[303.30694580078125,600.0020751953125,325.4039611816406,612.0070190429688],"content":"to the","score":1,"type":"text"},{"bbox":[326,602,333,610],"content":"x\\cdot","score":0.72,"type":"inline_equation"},{"bbox":[332.52294921875,600.0020751953125,558.4248657226562,612.0070190429688],"content":"-axis at early times to being mostly perpendicular to it af-","score":1,"type":"text"}]},{"bbox":[302,610.9600830078125,558,622.9650268554688],"spans":[{"bbox":[303.30694580078125,610.9600830078125,558.4290161132812,622.9650268554688],"content":"ter 5 Myr in the neighborhood of the dense layer. In this section,","score":1,"type":"text"}]},{"bbox":[302,621.9191284179688,427.25164794921875,633.924072265625],"spans":[{"bbox":[303.30694580078125,621.9191284179688,427.25164794921875,633.924072265625],"content":"we investigate how this occurs.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[303,653,505,664],"lines":[{"bbox":[303.30694580078125,652.6038818359375,504.53167724609375,664.3209228515625],"spans":[{"bbox":[303.30694580078125,652.6038818359375,504.53167724609375,664.3209228515625],"content":"4.1. Magnetic field amplification by MHD shocks","score":1,"type":"text"}]}],"type":"title"},{"bbox":[302,672.2571411132812,558,760.9750366210938],"lines":[{"bbox":[302,672.2571411132812,558,684.2620849609375],"spans":[{"bbox":[303.30694580078125,672.2571411132812,558.42919921875,684.2620849609375],"content":"As seen in Figure 2, and considering the shock front located at","score":1,"type":"text"}]},{"bbox":[302,683.2161254882812,558,695.2210693359375],"spans":[{"bbox":[303.30694580078125,683.2161254882812,558.42919921875,695.2210693359375],"content":"the right of the condensation layer, we see that the angle between","score":1,"type":"text"}]},{"bbox":[302,694.1751098632812,558,706.1800537109375],"spans":[{"bbox":[303.30694580078125,694.1751098632812,558.4292602539062,706.1800537109375],"content":"the upstream magnetic field and the normal to the shock front","score":1,"type":"text"}]},{"bbox":[302,705,558,717.1390991210938],"spans":[{"bbox":[303.30694580078125,705.1341552734375,334.8585205078125,717.1390991210938],"content":"satisfies","score":1,"type":"text"},{"bbox":[336,705,361,715],"content":"\\theta\\approx0","score":0.89,"type":"inline_equation"},{"bbox":[360.19122314453125,705.1341552734375,558.427001953125,717.1390991210938],"content":" for all the magnetic lines shown. The small vari-","score":1,"type":"text"}]},{"bbox":[302,716.0931396484375,558,728.0980834960938],"spans":[{"bbox":[303.30694580078125,716.0931396484375,337.97674560546875,728.0980834960938],"content":"ations of","score":1,"type":"text"},{"bbox":[337.97674560546875,717.5203857421875,344.9245300292969,727.4830322265625],"content":" θ","score":1,"type":"text"},{"bbox":[344.9245300292969,716.0931396484375,558.4246215820312,728.0980834960938],"content":" around zero are due to the fact that the shock front is","score":1,"type":"text"}]},{"bbox":[302,727.0521240234375,558,739.0570678710938],"spans":[{"bbox":[303.3069152832031,727.0521240234375,558.4290771484375,739.0570678710938],"content":"not a plane when it moves away from the central region because","score":1,"type":"text"}]},{"bbox":[302,738.0111083984375,558,750.0160522460938],"spans":[{"bbox":[303.3069152832031,738.0111083984375,558.428955078125,750.0160522460938],"content":"of the fluctuations added to the inflow velocity in the simulation","score":1,"type":"text"}]},{"bbox":[302,748.9700927734375,326,760.9750366210938],"spans":[{"bbox":[303.3069152832031,748.9700927734375,326.82861328125,760.9750366210938],"content":"setup.","score":1,"type":"text"}]}],"type":"text"}]},{"discarded_blocks":[{"bbox":[241,34,355,42],"lines":[{"bbox":[240.98399353027344,32.58107376098633,354.29205322265625,43.38558578491211],"spans":[{"bbox":[240.98399353027344,32.58107376098633,247.45773315429688,43.38558578491211],"content":"A","score":1,"type":"text"},{"bbox":[247.45700073242188,34.06907653808594,254.432861328125,43.03547668457031],"content":"&","score":1,"type":"text"},{"bbox":[254.43299865722656,32.58107376098633,288.55010986328125,43.38558578491211],"content":"A proofs:","score":1,"type":"text"},{"bbox":[288.55010986328125,32.58107376098633,354.29205322265625,43.38558578491211],"content":" manuscript no. aa","score":1,"type":"text"}]}],"type":"discarded"},{"bbox":[36,771,139,779],"lines":[{"bbox":[36.849700927734375,769.81591796875,140.07986450195312,780.6204223632812],"spans":[{"bbox":[36.849700927734375,769.81591796875,140.07986450195312,780.6204223632812],"content":"Article number, page 4 of 11","score":1,"type":"text"}]}],"type":"discarded"}],"page_idx":3,"page_size":[595.2760009765625,841.8900146484375],"preproc_blocks":[{"bbox":[33,84,560,344],"blocks":[{"bbox":[33,84,553,303],"lines":[{"bbox":[33,84,553,303],"spans":[{"bbox":[33,84,553,303],"image_path":"f58693ef236783809189fc9ccee7f9b0cfc65496fed0f0ca6bee2a745507dd5b.jpg","score":0.9997164011001587,"type":"image"}]}],"type":"image_body"},{"bbox":[36,322,560,344],"lines":[{"bbox":[36.849998474121094,322.947265625,558.4275512695312,334.6125793457031],"spans":[{"bbox":[36.849998474121094,322.947265625,61.39103698730469,334.6125793457031],"content":"Fig. 1.","score":1,"type":"text"},{"bbox":[61.39103698730469,323.27008056640625,558.4275512695312,334.0745849609375],"content":" Column density of the cold atomic cloud’s simulation at 5 Myr. 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The downstream","score":1,"type":"text"}]},{"bbox":[35,497.36651611328125,291,509.3714599609375],"spans":[{"bbox":[36.850006103515625,497.36651611328125,291.9722900390625,509.3714599609375],"content":"flow, just after the shock front, becomes transalfvénic as we can","score":1,"type":"text"}]},{"bbox":[35,508.32550048828125,291,520.3304443359375],"spans":[{"bbox":[36.850006103515625,508.32550048828125,198.93157958984375,520.3304443359375],"content":"see from Figure 2. Therefore the relation","score":1,"type":"text"},{"bbox":[200,509,263,520],"content":"u_{f}>|u_{n}|>u_{A,n}","score":0.94,"type":"inline_equation"},{"bbox":[262.69195556640625,508.32550048828125,291.9720153808594,520.3304443359375],"content":", which","score":1,"type":"text"}]},{"bbox":[35,519.2844848632812,245.88519287109375,531.2894287109375],"spans":[{"bbox":[36.84996032714844,519.2844848632812,245.88519287109375,531.2894287109375],"content":"characterizes a subfast flow, is satisfied downstream.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[35,531.407470703125,291,587.2483520507812],"lines":[{"bbox":[51,531.407470703125,291,543.4124145507812],"spans":[{"bbox":[51.79396057128906,531.407470703125,291.9722900390625,543.4124145507812],"content":"Such MHD shock, going from a superfast to a subfast flow,","score":1,"type":"text"}]},{"bbox":[35,542.366455078125,291,554.3713989257812],"spans":[{"bbox":[36.84996032714844,542.366455078125,291.9721984863281,554.3713989257812],"content":"is called a fast MHD shock (Delmont & Keppens 2011), whose","score":1,"type":"text"}]},{"bbox":[35,553.325439453125,291,565.3303833007812],"spans":[{"bbox":[36.84996032714844,553.325439453125,291.97222900390625,565.3303833007812],"content":"main feature is that it refracts the magnetic field away from the","score":1,"type":"text"}]},{"bbox":[35,564.284423828125,291,576.2893676757812],"spans":[{"bbox":[36.84996032714844,564.284423828125,291.9721984863281,576.2893676757812],"content":"shock normal due to the amplification of the magnetic field com-","score":1,"type":"text"}]},{"bbox":[35,575.243408203125,291,587.2483520507812],"spans":[{"bbox":[36.84996032714844,575.243408203125,291.9721984863281,587.2483520507812],"content":"ponent parallel to the shock front. This amplification is given by","score":1,"type":"text"}]}],"type":"text"},{"bbox":[34,606,152,640],"lines":[{"bbox":[34,606,152,640],"spans":[{"bbox":[34,606,152,640],"content":"B_{\\parallel,2}=\\frac{r_{\\rho}B_{\\parallel,1}(M_{A,1}^{2}-\\cos^{2}\\theta)}{M_{A,1}^{2}-r_{\\rho}\\cos^{2}\\theta},","score":0.93,"type":"interline_equation"}]}],"type":"interline_equation"},{"bbox":[35,650.340576171875,291,760.9755249023438],"lines":[{"bbox":[35,650.340576171875,291,663.8395385742188],"spans":[{"bbox":[36.84999084472656,650.340576171875,61.188621520996094,662.3455200195312],"content":"where","score":1,"type":"text"},{"bbox":[62,651,101,662],"content":"B_{\\parallel,1}=B_{1}","score":0.7,"type":"inline_equation"},{"bbox":[100.79489135742188,650.340576171875,114.5803451538086,663.8395385742188],"content":" sin","score":1,"type":"text"},{"bbox":[115,651,121,660],"content":"\\theta","score":0.26,"type":"inline_equation"},{"bbox":[120.61357879638672,650.340576171875,137.7509765625,662.3455200195312],"content":" and","score":1,"type":"text"},{"bbox":[139,651,155,662],"content":"B_{\\parallel,2}","score":0.9,"type":"inline_equation"},{"bbox":[154.71788024902344,650.340576171875,291.96343994140625,663.8395385742188],"content":" are the upstream and downstream","score":1,"type":"text"}]},{"bbox":[35,661.299560546875,291,673.3045043945312],"spans":[{"bbox":[36.84998321533203,661.299560546875,247.74826049804688,673.3045043945312],"content":"magnetic field components parallel to the shock front,","score":1,"type":"text"},{"bbox":[248,662,291,673],"content":"r_{\\rho}=\\rho_{2}/\\rho_{1}","score":0.91,"type":"inline_equation"}]},{"bbox":[35,672.258544921875,291,684.2634887695312],"spans":[{"bbox":[36.850006103515625,672.258544921875,157.5967254638672,684.2634887695312],"content":"is the ratio of the downstream","score":1,"type":"text"},{"bbox":[159,673,176,684],"content":"(\\rho_{2})","score":0.87,"type":"inline_equation"},{"bbox":[176.2245635986328,672.258544921875,235.98023986816406,684.2634887695312],"content":" and upstream ","score":1,"type":"text"},{"bbox":[235,673,251,684],"content":"(\\rho_{1})","score":0.85,"type":"inline_equation"},{"bbox":[251.6605682373047,672.258544921875,291.96923828125,684.2634887695312],"content":" densities,","score":1,"type":"text"}]},{"bbox":[35,683,291,696.7164916992188],"spans":[{"bbox":[35,683,55,695],"content":"M_{A,1}","score":0.91,"type":"inline_equation"},{"bbox":[55.312923431396484,683.216552734375,275.6275329589844,696.7164916992188],"content":" is the Alfvénic Mach number of the upstream gas, and","score":1,"type":"text"},{"bbox":[275.6275329589844,684.643798828125,278.2190246582031,694.6064453125],"content":" ","score":1,"type":"text"},{"bbox":[277,684,283,693],"content":"\\theta","score":0.73,"type":"inline_equation"},{"bbox":[282.5926208496094,683.216552734375,291.96807861328125,695.2214965820312],"content":" is","score":1,"type":"text"}]},{"bbox":[35,694.1755981445312,291,706.1805419921875],"spans":[{"bbox":[36.85002136230469,694.1755981445312,291.9722595214844,706.1805419921875],"content":"the angle between the vector normal to the front-shock and the","score":1,"type":"text"}]},{"bbox":[35,705,291,717.1395263671875],"spans":[{"bbox":[36.85002136230469,705.1345825195312,131.99282836914062,717.1395263671875],"content":"upstream magnetic field","score":1,"type":"text"},{"bbox":[133,705,147,716],"content":"B_{1}","score":0.88,"type":"inline_equation"},{"bbox":[146.79803466796875,705.1345825195312,291.9730224609375,717.1395263671875],"content":". Since this amplification depends on","score":1,"type":"text"}]},{"bbox":[35,716.0935668945312,291,728.0985107421875],"spans":[{"bbox":[36.85003662109375,716.0935668945312,73.0840072631836,728.0985107421875],"content":"the angle","score":1,"type":"text"},{"bbox":[74,717,80,726],"content":"\\theta","score":0.69,"type":"inline_equation"},{"bbox":[80.0860366821289,716.0935668945312,275.1337585449219,728.0985107421875],"content":", the fluctuating curvature of the shock front at di","score":1,"type":"text"},{"bbox":[275.1320495605469,717.7468872070312,281.109619140625,727.70947265625],"content":"ff","score":1,"type":"text"},{"bbox":[281.1090393066406,716.0935668945312,291.96826171875,728.0985107421875],"content":"er-","score":1,"type":"text"}]},{"bbox":[35,727.0526123046875,291,739.0575561523438],"spans":[{"bbox":[36.85003662109375,727.0526123046875,291.97222900390625,739.0575561523438],"content":"ent positions yields the inhomogeneous downstream magnetic","score":1,"type":"text"}]},{"bbox":[35,738.0115966796875,291,750.0165405273438],"spans":[{"bbox":[36.85003662109375,738.0115966796875,291.9723205566406,750.0165405273438],"content":"field pattern when the shock front travels away from the central","score":1,"type":"text"}]},{"bbox":[35,748.9705810546875,236.03228759765625,760.9755249023438],"spans":[{"bbox":[36.85003662109375,748.9705810546875,236.03228759765625,760.9755249023438],"content":"region, early in the evolution times (see Figure 2).","score":1,"type":"text"}]}],"type":"text"},{"bbox":[302,362.3353271484375,413.41705322265625,374.0523986816406],"lines":[{"bbox":[302,362.3353271484375,413.41705322265625,374.0523986816406],"spans":[{"bbox":[303.3070373535156,362.3353271484375,413.41705322265625,374.0523986816406],"content":"4.2. Line bending analysis","score":1,"type":"text"}]}],"type":"text"},{"bbox":[302,379.50457763671875,558,413.426513671875],"lines":[{"bbox":[302,379.50457763671875,558,391.509521484375],"spans":[{"bbox":[303.3070373535156,379.50457763671875,558.4293212890625,391.509521484375],"content":"To understand how magnetic field lines change their original di-","score":1,"type":"text"}]},{"bbox":[302,390.46258544921875,558,402.467529296875],"spans":[{"bbox":[303.3070373535156,390.46258544921875,558.4292602539062,402.467529296875],"content":"rection in the post-shock region, we consider the induction equa-","score":1,"type":"text"}]},{"bbox":[302,401.42156982421875,379.1323547363281,413.426513671875],"spans":[{"bbox":[303.3070373535156,401.42156982421875,379.1323547363281,413.426513671875],"content":"tion in ideal MHD,","score":1,"type":"text"}]}],"type":"text"},{"bbox":[302,418,465,443],"lines":[{"bbox":[302,418,465,443],"spans":[{"bbox":[302,418,465,443],"content":"\\frac{\\partial\\pmb{B}}{\\partial t}=-\\pmb{B}\\nabla\\cdot\\pmb{u}-(\\pmb{u}\\cdot\\nabla)\\pmb{B}+(\\pmb{B}\\cdot\\nabla)\\pmb{u}.","score":0.93,"type":"interline_equation"}]}],"type":"interline_equation"},{"bbox":[303,458,480,469],"lines":[{"bbox":[303.306884765625,457.82830810546875,479.6495056152344,469.5453796386719],"spans":[{"bbox":[303.306884765625,457.82830810546875,479.6495056152344,469.5453796386719],"content":"4.2.1. Line bending by a compressive flow","score":1,"type":"text"}]}],"type":"title"},{"bbox":[302,474.99755859375,558,563.7153930664062],"lines":[{"bbox":[302,474.99755859375,558,487.00250244140625],"spans":[{"bbox":[303.306884765625,474.99755859375,558.4292602539062,487.00250244140625],"content":"This analysis takes place after the magnetic field component par-","score":1,"type":"text"}]},{"bbox":[302,485.95654296875,558,497.96148681640625],"spans":[{"bbox":[303.306884765625,485.95654296875,558.4290161132812,497.96148681640625],"content":"allel to the shock front is amplified by the fast MHD shock, i.e.,","score":1,"type":"text"}]},{"bbox":[302,496.91552734375,558,508.92047119140625],"spans":[{"bbox":[303.306884765625,496.91552734375,558.4290161132812,508.92047119140625],"content":"in a region containing cooling and thermally unstable gas. Af-","score":1,"type":"text"}]},{"bbox":[302,507.87451171875,558,519.8794555664062],"spans":[{"bbox":[303.306884765625,507.87451171875,558.4292602539062,519.8794555664062],"content":"ter the amplification, magnetic field lines adopt the shape repre-","score":1,"type":"text"}]},{"bbox":[302,518.83349609375,558,530.8384399414062],"spans":[{"bbox":[303.306884765625,518.83349609375,558.42919921875,530.8384399414062],"content":"sented in Figure 5, where the magnetic field component parallel","score":1,"type":"text"}]},{"bbox":[302,529.79248046875,558,541.7974243164062],"spans":[{"bbox":[303.306884765625,529.79248046875,375.05743408203125,541.7974243164062],"content":"to the shock front,","score":1,"type":"text"},{"bbox":[376,530,387,541],"content":"B_{y}","score":0.86,"type":"inline_equation"},{"bbox":[387.2288818359375,529.79248046875,558.4262084960938,541.7974243164062],"content":", has been amplified, and the magnetic field","score":1,"type":"text"}]},{"bbox":[302,540.75146484375,558,554.2504272460938],"spans":[{"bbox":[303.306884765625,540.75146484375,475.9286804199219,552.7564086914062],"content":"component perpendicular to the shock front","score":1,"type":"text"},{"bbox":[477,541,489,552],"content":"B_{x}","score":0.88,"type":"inline_equation"},{"bbox":[487.91326904296875,540.75146484375,558.4244384765625,554.2504272460938],"content":" stays constant, in","score":1,"type":"text"}]},{"bbox":[302,551.71044921875,533.2536010742188,563.7153930664062],"spans":[{"bbox":[303.306884765625,551.71044921875,533.2536010742188,563.7153930664062],"content":"agreement with the jump condition for the magnetic field.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[302,562.66845703125,558,761],"lines":[{"bbox":[318.2508850097656,562.66845703125,558,574.6734008789062],"spans":[{"bbox":[318.2508850097656,562.66845703125,558.42919921875,574.6734008789062],"content":"Furthermore, we assume that the flow speed decreases along","score":1,"type":"text"}]},{"bbox":[302,573.62744140625,558,585.6323852539062],"spans":[{"bbox":[302,576,309,583],"content":"x","score":0.72,"type":"inline_equation"},{"bbox":[308.228271484375,573.62744140625,433.30572509765625,585.6323852539062],"content":" in the post-shock region; i.e.,","score":1,"type":"text"},{"bbox":[433.30572509765625,573.62744140625,437.1528625488281,585.5227661132812],"content":" ","score":1,"type":"text"},{"bbox":[436,574,484,585],"content":"u_{x}~=~u_{x}(x)","score":0.92,"type":"inline_equation"},{"bbox":[483.5093688964844,573.62744140625,501.74090576171875,585.6323852539062],"content":" and","score":1,"type":"text"},{"bbox":[501.74090576171875,575.0546875,505.58184814453125,585.017333984375],"content":" ","score":1,"type":"text"},{"bbox":[504,574,556,585],"content":"\\partial u_{x}/\\partial x\\ <\\ 0","score":0.92,"type":"inline_equation"},{"bbox":[555.9341430664062,573.62744140625,558.4248046875,585.6323852539062],"content":",","score":1,"type":"text"}]},{"bbox":[302,584.58642578125,558,596.5913696289062],"spans":[{"bbox":[303.30682373046875,584.58642578125,558.4291381835938,596.5913696289062],"content":"which represents the compression caused by the cooling of the","score":1,"type":"text"}]},{"bbox":[302,595.54541015625,558,607.5503540039062],"spans":[{"bbox":[303.30682373046875,595.54541015625,558.4291381835938,607.5503540039062],"content":"gas as it travels downstream. Finally, we disregard the down-","score":1,"type":"text"}]},{"bbox":[302,606.5044555664062,558,618.5093994140625],"spans":[{"bbox":[303.30682373046875,606.5044555664062,547.0120239257812,618.5093994140625],"content":"stream component of the velocity parallel to the shock front,","score":1,"type":"text"},{"bbox":[547.0120239257812,606.5044555664062,549.8488159179688,618.3997802734375],"content":" ","score":1,"type":"text"},{"bbox":[549,608,559,618],"content":"u_{y}","score":0.83,"type":"inline_equation"}]},{"bbox":[302,617.4634399414062,558,629.4683837890625],"spans":[{"bbox":[303.30682373046875,617.4634399414062,317.69281005859375,629.4683837890625],"content":"and","score":1,"type":"text"},{"bbox":[319,619,329,629],"content":"u_{z}","score":0.86,"type":"inline_equation"},{"bbox":[329.02081298828125,617.4634399414062,398.8287353515625,629.4683837890625],"content":", to analyze the e","score":1,"type":"text"},{"bbox":[398.82781982421875,619.1167602539062,404.8053894042969,629.079345703125],"content":"ff","score":1,"type":"text"},{"bbox":[404.8048095703125,617.4634399414062,558.4281616210938,629.4683837890625],"content":"ect of the compression alone. To vali-","score":1,"type":"text"}]},{"bbox":[302,628.4224243164062,558,640.4273681640625],"spans":[{"bbox":[303.30682373046875,628.4224243164062,558.4290161132812,640.4273681640625],"content":"date these assumptions, in Figure 6 we plot the relevant physical","score":1,"type":"text"}]},{"bbox":[302,639.3814697265625,558,651.3864135742188],"spans":[{"bbox":[303.30682373046875,639.3814697265625,373.01507568359375,651.3864135742188],"content":"quantities at time","score":1,"type":"text"},{"bbox":[373.01507568359375,639.3814697265625,376.04083251953125,651.2767944335938],"content":" ","score":1,"type":"text"},{"bbox":[375,640,405,650],"content":"t=0.7","score":0.8,"type":"inline_equation"},{"bbox":[405.3020935058594,639.3814697265625,531.3687744140625,651.3864135742188],"content":" Myr along a ray parallel to the","score":1,"type":"text"},{"bbox":[533,641,540,650],"content":"x","score":0.79,"type":"inline_equation"},{"bbox":[539.3181762695312,639.3814697265625,558.4244995117188,651.3864135742188],"content":" axis","score":1,"type":"text"}]},{"bbox":[302,650.3404541015625,558,662.3453979492188],"spans":[{"bbox":[303.3067626953125,650.3404541015625,558.428955078125,662.3453979492188],"content":"passing through a region in which this amplification becomes","score":1,"type":"text"}]},{"bbox":[302,661.2994384765625,558,673.3043823242188],"spans":[{"bbox":[303.3067626953125,661.2994384765625,558.428955078125,673.3043823242188],"content":"large at later evolutionary times. In the top panel, the shock front","score":1,"type":"text"}]},{"bbox":[302,672.2574462890625,558,684.2623901367188],"spans":[{"bbox":[303.3067626953125,672.2574462890625,558.4288940429688,684.2623901367188],"content":"and condensed region are clearly visible in the gas density pro-","score":1,"type":"text"}]},{"bbox":[302,683.2164306640625,558,695.2213745117188],"spans":[{"bbox":[303.3067626953125,683.2164306640625,558.4290771484375,695.2213745117188],"content":"file. The middle panel shows that, in addition to the discontinuity","score":1,"type":"text"}]},{"bbox":[302,694.1754150390625,558,707.6753540039062],"spans":[{"bbox":[303.3067626953125,694.1754150390625,436.84539794921875,706.1803588867188],"content":"at the shocks, the inflow velocity","score":1,"type":"text"},{"bbox":[438,696,450,705],"content":"u_{x}","score":0.85,"type":"inline_equation"},{"bbox":[448.3121032714844,694.1754150390625,558.4247436523438,707.6753540039062],"content":" smoothly decreases down-","score":1,"type":"text"}]},{"bbox":[302,705.1344604492188,558,717.139404296875],"spans":[{"bbox":[303.3067321777344,705.1344604492188,558.428955078125,717.139404296875],"content":"stream from the shock, in sync with the density increase. Also,","score":1,"type":"text"}]},{"bbox":[302,716.0934448242188,558,728.098388671875],"spans":[{"bbox":[302,718,312,728],"content":"u_{y}","score":0.71,"type":"inline_equation"},{"bbox":[311.8827209472656,717.5206909179688,314.3733825683594,727.4833374023438],"content":",","score":1,"type":"text"},{"bbox":[314.3733825683594,716.0934448242188,319.3457336425781,727.98876953125],"content":" ","score":1,"type":"text"},{"bbox":[318,717,348,727],"content":"u_{z}\\,\\approx\\,0","score":0.89,"type":"inline_equation"},{"bbox":[347.4330139160156,716.0934448242188,482.147216796875,728.098388671875],"content":", in agreement with our assumpti","score":1,"type":"text"},{"bbox":[495.9852600097656,716.0934448242188,558.4208984375,728.098388671875],"content":". Finally, in the","score":1,"type":"text"}]},{"bbox":[302,727,558,740.5513916015625],"spans":[{"bbox":[303.3067321777344,727.0524291992188,481.1788635253906,739.057373046875],"content":"bottom panel, we see that the fluctuation of","score":1,"type":"text"},{"bbox":[483,727,495,738],"content":"B_{x}","score":0.89,"type":"inline_equation"},{"bbox":[494.2731018066406,727.0524291992188,558.4292602539062,740.5513916015625],"content":" remains within","score":1,"type":"text"}]},{"bbox":[302,738,558,750.0164184570312],"spans":[{"bbox":[302,738,333,749],"content":"\\lesssim\\,20\\%","score":0.89,"type":"inline_equation"},{"bbox":[332.7591552734375,738.011474609375,558.421875,750.0164184570312],"content":" of its mean value, so it is negligible to the first order.","score":1,"type":"text"}]},{"bbox":[302,748.970458984375,558,761],"spans":[{"bbox":[303.30670166015625,748.970458984375,413.0945129394531,760.9754028320312],"content":"Therefore, the assumptions","score":1,"type":"text"},{"bbox":[413.0945129394531,748.970458984375,416.74169921875,760.8657836914062],"content":" ","score":1,"type":"text"},{"bbox":[415,749,463,761],"content":"B_{y}\\,=\\,B_{y}(x)","score":0.76,"type":"inline_equation"},{"bbox":[462.6882629394531,748.970458984375,465.1789245605469,760.9754028320312],"content":",","score":1,"type":"text"},{"bbox":[465.1789245605469,748.970458984375,468.8227233886719,760.8657836914062],"content":" ","score":1,"type":"text"},{"bbox":[467,749,500,760],"content":"B_{x}\\,=\\,C","score":0.59,"type":"inline_equation"},{"bbox":[500.4847412109375,748.970458984375,530.6116943359375,760.9754028320312],"content":", where","score":1,"type":"text"},{"bbox":[530.6116943359375,748.970458984375,533.6547241210938,760.8657836914062],"content":" ","score":1,"type":"text"},{"bbox":[533,749,541,759],"content":"C","score":0.78,"type":"inline_equation"},{"bbox":[540.2998046875,748.970458984375,558.427734375,760.9754028320312],"content":" is a","score":1,"type":"text"}]}],"type":"text"}]},{"discarded_blocks":[{"bbox":[174,34,420,43],"lines":[{"bbox":[174.968994140625,32.58107376098633,420.3074951171875,43.38558578491211],"spans":[{"bbox":[174.968994140625,32.58107376098633,420.3074951171875,43.38558578491211],"content":"Granda-Muñoz et al.: Magnetic field alignment in interstellar clouds","score":1,"type":"text"}]}],"type":"discarded"},{"bbox":[456,771,558,779],"lines":[{"bbox":[455.1949157714844,769.8160400390625,558.4251098632812,780.6205444335938],"spans":[{"bbox":[455.1949157714844,769.8160400390625,558.4251098632812,780.6205444335938],"content":"Article number, page 5 of 11","score":1,"type":"text"}]}],"type":"discarded"}],"page_idx":4,"page_size":[595.2760009765625,841.8900146484375],"preproc_blocks":[{"bbox":[37,54,558,419],"blocks":[{"bbox":[92,54,503,363],"lines":[{"bbox":[92,54,503,363],"spans":[{"bbox":[92,54,503,363],"image_path":"70d48a8caa72e2a1fb2dba440b843dccd872512362f2236fb151e9e6e515c87a.jpg","score":0.9999694228172302,"type":"image"}]}],"type":"image_body"},{"bbox":[37,370,558,419],"lines":[{"bbox":[36.849998474121094,369.34027099609375,558.4281616210938,381.0055847167969],"spans":[{"bbox":[36.849998474121094,369.34027099609375,60.386802673339844,381.0055847167969],"content":"Fig. 2.","score":1,"type":"text"},{"bbox":[60.386802673339844,369.6630859375,558.4281616210938,380.46759033203125],"content":" The density structure and magnetic field lines of the region R1 are shown after 5 Myr of evolution. The magnetic field lines are colored by","score":1,"type":"text"}]},{"bbox":[36.849998474121094,379.6260986328125,558.42529296875,390.43060302734375],"spans":[{"bbox":[36.849998474121094,379.6260986328125,558.42529296875,390.43060302734375],"content":"the Alfvénic Mach number. Note that at this evolution time, magnetic field lines are almost perpendicular to their original orientation along the","score":1,"type":"text"}]},{"bbox":[36,389.589111328125,558.4230346679688,400.39361572265625],"spans":[{"bbox":[36,391,42,398],"content":"x","score":0.73,"type":"inline_equation"},{"bbox":[41.28008270263672,389.589111328125,558.4230346679688,400.39361572265625],"content":" axis and the change from superalfvénic to transalfvénic of magnetic field lines across the shock. The dark-shaded regions at both sides of the","score":1,"type":"text"}]},{"bbox":[36.849998474121094,399.5511169433594,558.4254760742188,410.3556213378906],"spans":[{"bbox":[36.849998474121094,399.5511169433594,558.4254760742188,410.3556213378906],"content":"center are the shock fronts where magnetic field lines start to bend. 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(7) implies that","score":1,"type":"text"},{"bbox":[210,550,239,561],"content":"d B_{y}/d t","score":0.9,"type":"inline_equation"},{"bbox":[238.99288940429688,549.8035888671875,291.971435546875,561.8085327148438],"content":" has the same","score":1,"type":"text"}]},{"bbox":[36,560.7625732421875,291,574.2615356445312],"spans":[{"bbox":[36.850006103515625,560.7625732421875,64.45636749267578,572.7675170898438],"content":"sign as","score":1,"type":"text"},{"bbox":[64.45636749267578,560.7625732421875,67.50200653076172,572.6578979492188],"content":" ","score":1,"type":"text"},{"bbox":[66,561,77,573],"content":"B_{y}","score":0.87,"type":"inline_equation"},{"bbox":[77.0840072631836,560.7625732421875,256.7893371582031,572.7675170898438],"content":", and therefore the magnetic field component","score":1,"type":"text"},{"bbox":[258,561,269,573],"content":"B_{y}","score":0.88,"type":"inline_equation"},{"bbox":[268.91839599609375,560.7625732421875,291.970458984375,574.2615356445312],"content":" is al-","score":1,"type":"text"}]},{"bbox":[36,571.7215576171875,291,583.7265014648438],"spans":[{"bbox":[36.85002136230469,571.7215576171875,291.97222900390625,583.7265014648438],"content":"ways amplified by the downstream compressive velocity gradi-","score":1,"type":"text"}]},{"bbox":[36,582.6795654296875,291,594.6845092773438],"spans":[{"bbox":[36.85002136230469,582.6795654296875,291.9722595214844,594.6845092773438],"content":"ent. This amplification results in the magnetic field aligning to","score":1,"type":"text"}]},{"bbox":[36,593.6385498046875,205.7858123779297,605.6434936523438],"spans":[{"bbox":[36.85002136230469,593.6385498046875,205.7858123779297,605.6434936523438],"content":"the condensation plane where CACs form.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[36,623,203,633],"lines":[{"bbox":[36.85002136230469,622.0263671875,203.02777099609375,633.743408203125],"spans":[{"bbox":[36.85002136230469,622.0263671875,203.02777099609375,633.743408203125],"content":"4.2.2. Line bending at curved interfaces","score":1,"type":"text"}]}],"type":"title"},{"bbox":[36,639.381591796875,291,760.9755249023438],"lines":[{"bbox":[36,639.381591796875,291,651.3865356445312],"spans":[{"bbox":[36.85002136230469,639.381591796875,291.9722595214844,651.3865356445312],"content":"Another possible mechanism for aligning the magnetic field","score":1,"type":"text"}]},{"bbox":[36,650.340576171875,291,662.3455200195312],"spans":[{"bbox":[36.85002136230469,650.340576171875,291.9722595214844,662.3455200195312],"content":"with the density structures occurs when the collision interface","score":1,"type":"text"}]},{"bbox":[36,661.299560546875,291,673.3045043945312],"spans":[{"bbox":[36.85002136230469,661.299560546875,291.9722900390625,673.3045043945312],"content":"is curved rather than flat, as, for example, in the case of the","score":1,"type":"text"}]},{"bbox":[36,672.258544921875,291,684.2634887695312],"spans":[{"bbox":[36.85002136230469,672.258544921875,291.97222900390625,684.2634887695312],"content":"NTSI (Vishniac 1994). To investigate this, we also ran two-","score":1,"type":"text"}]},{"bbox":[36,683.216552734375,291,695.2214965820312],"spans":[{"bbox":[36.85002136230469,683.216552734375,291.9722900390625,695.2214965820312],"content":"dimensional simulations with the same initial conditions and","score":1,"type":"text"}]},{"bbox":[36,694.175537109375,291,706.1804809570312],"spans":[{"bbox":[36.85002136230469,694.175537109375,291.9722900390625,706.1804809570312],"content":"physics as the three-dimensional simulation described in Sec-","score":1,"type":"text"}]},{"bbox":[36,705.134521484375,291,717.1394653320312],"spans":[{"bbox":[36.85002136230469,705.134521484375,291.9722595214844,717.1394653320312],"content":"tion 2 but with a curved collision interface, obtained by adding","score":1,"type":"text"}]},{"bbox":[36,716.0935668945312,291,728.0985107421875],"spans":[{"bbox":[36.85002136230469,716.0935668945312,291.9722595214844,728.0985107421875],"content":"a sinusoidal displacement perturbation (a “bending mode” per-","score":1,"type":"text"}]},{"bbox":[36,727.0525512695312,291,739.0574951171875],"spans":[{"bbox":[36.85002136230469,727.0525512695312,291.9721984863281,739.0574951171875],"content":"turbation). In the left panel of Figure 7, we show a very early","score":1,"type":"text"}]},{"bbox":[36,738.0115356445312,291,750.0164794921875],"spans":[{"bbox":[36.85002136230469,738.0115356445312,291.9721984863281,750.0164794921875],"content":"stage of this simulation. In this case, the obliqueness of the in-","score":1,"type":"text"}]},{"bbox":[36,748.9705810546875,291,760.9755249023438],"spans":[{"bbox":[36.85002136230469,748.9705810546875,291.9722595214844,760.9755249023438],"content":"terface implies the existence of a component of the incoming","score":1,"type":"text"}]},{"bbox":[303,436.5965576171875,558,448.60150146484375],"spans":[{"bbox":[303.3070068359375,436.5965576171875,558.4292602539062,448.60150146484375],"content":"flow tangential to it, while the perpendicular component is re-","score":1,"type":"text"}]},{"bbox":[303,447.5555419921875,558,459.56048583984375],"spans":[{"bbox":[303.3070068359375,447.5555419921875,558.4293823242188,459.56048583984375],"content":"duced across the shock. This causes the flow to change direction","score":1,"type":"text"}]},{"bbox":[303,458.5145263671875,558,470.51947021484375],"spans":[{"bbox":[303.3070068359375,458.5145263671875,558.4290161132812,470.51947021484375],"content":"at the interface, being now oblique to the original magnetic field","score":1,"type":"text"}]},{"bbox":[303,469.4725341796875,558,481.47747802734375],"spans":[{"bbox":[303.3070068359375,469.4725341796875,558.4290771484375,481.47747802734375],"content":"direction. Being transalfvénic, this oblique post-shock flow can","score":1,"type":"text"}]},{"bbox":[303,480.4315185546875,558,492.43646240234375],"spans":[{"bbox":[303.3070068359375,480.4315185546875,558.4293212890625,492.43646240234375],"content":"begin bending the field lines. The situation is symmetric on both","score":1,"type":"text"}]},{"bbox":[303,491.3905029296875,558,503.39544677734375],"spans":[{"bbox":[303.3070068359375,491.3905029296875,558.4291381835938,503.39544677734375],"content":"sides of the layer, thus generating a shearing velocity field with","score":1,"type":"text"}]},{"bbox":[303,502.3494873046875,558,514.3544311523438],"spans":[{"bbox":[303.3070068359375,502.3494873046875,498.7630920410156,514.3544311523438],"content":"opposite directions at opposite sides due to the di","score":1,"type":"text"},{"bbox":[498.76702880859375,504.0028076171875,504.7445983886719,513.9653930664062],"content":"ff","score":1,"type":"text"},{"bbox":[504.7450256347656,502.3494873046875,558.423583984375,514.3544311523438],"content":"erent concav-","score":1,"type":"text"}]},{"bbox":[303,513.3084716796875,558,525.3134155273438],"spans":[{"bbox":[303.3070068359375,513.3084716796875,558.42919921875,525.3134155273438],"content":"ity of the collision interface. This generates an “S” shape of the","score":1,"type":"text"}]},{"bbox":[303,524.2674560546875,558,536.2723999023438],"spans":[{"bbox":[303.3070068359375,524.2674560546875,558.4293212890625,536.2723999023438],"content":"magnetic field lines across the shocked layer. A later stage of","score":1,"type":"text"}]},{"bbox":[303,535.2264404296875,558,547.2313842773438],"spans":[{"bbox":[303.3070068359375,535.2264404296875,558.4291381835938,547.2313842773438],"content":"this simulation is shown in the right panel of Figure 7, showing","score":1,"type":"text"}]},{"bbox":[303,546.1854248046875,558,558.1903686523438],"spans":[{"bbox":[303.3070068359375,546.1854248046875,558.4293823242188,558.1903686523438],"content":"that the flow tends to be subalfvénic in the condensed regions.","score":1,"type":"text"}]},{"bbox":[303,557.1444091796875,558,569.1493530273438],"spans":[{"bbox":[303.3070068359375,557.1444091796875,519.4454345703125,569.1493530273438],"content":"For this collision interface, the line-bending analysis di","score":1,"type":"text"},{"bbox":[519.447998046875,558.7977294921875,525.425537109375,568.7603149414062],"content":"ff","score":1,"type":"text"},{"bbox":[525.426025390625,557.1444091796875,558.4222412109375,569.1493530273438],"content":"ers from","score":1,"type":"text"}]},{"bbox":[303,568.1033935546875,558,580.1083374023438],"spans":[{"bbox":[303.3070068359375,568.1033935546875,558.4293823242188,580.1083374023438],"content":"that described in Section 4.2. 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In this work, we identified that it is the action of","score":1,"type":"text"}]},{"bbox":[303,380.85028076171875,558,392.855224609375],"spans":[{"bbox":[303.3070068359375,380.85028076171875,558.4292602539062,392.855224609375],"content":"a fast MHD shock and the compressive velocity resulting from","score":1,"type":"text"}]},{"bbox":[303,391.80926513671875,543,403.814208984375],"spans":[{"bbox":[303.3070068359375,391.80926513671875,507.73956298828125,403.814208984375],"content":"the gas settlement onto the dense layer that leads to","score":1,"type":"text"},{"bbox":[507.73956298828125,393.2365417480469,510.23101806640625,403.1991271972656],"content":" ","score":1,"type":"text"},{"bbox":[509,392,541,403],"content":"\\phi=90^{\\circ}","score":0.91,"type":"inline_equation"},{"bbox":[541.508056640625,391.80926513671875,543.9987182617188,403.814208984375],"content":".","score":1,"type":"text"}]}],"type":"text"},{"bbox":[303,404.4152526855469,558,591.7630004882812],"lines":[{"bbox":[318,404.4152526855469,558,416.4201965332031],"spans":[{"bbox":[318.25103759765625,404.4152526855469,558.4293212890625,416.4201965332031],"content":"Since we have focused on non-gravitational CACs, we have","score":1,"type":"text"}]},{"bbox":[303,415.374267578125,558,427.37921142578125],"spans":[{"bbox":[303.3070373535156,415.374267578125,422.1806335449219,427.37921142578125],"content":"not numerically explored how","score":1,"type":"text"},{"bbox":[423,416,430,426],"content":"\\phi","score":0.83,"type":"inline_equation"},{"bbox":[429.969482421875,415.374267578125,467.13922119140625,427.37921142578125],"content":" becomes","score":1,"type":"text"},{"bbox":[468,416,478,425],"content":"0^{\\circ}","score":0.82,"type":"inline_equation"},{"bbox":[478.39605712890625,415.374267578125,558.4257202148438,427.37921142578125],"content":". However, a discus-","score":1,"type":"text"}]},{"bbox":[303,426.333251953125,558,438.33819580078125],"spans":[{"bbox":[303.30706787109375,426.333251953125,558.42919921875,438.33819580078125],"content":"sion similar to that in Section 4.2.1 leads us to speculate that the","score":1,"type":"text"}]},{"bbox":[303,437,558,449.29718017578125],"spans":[{"bbox":[302,437,329,448],"content":"\\phi=0^{\\circ}","score":0.91,"type":"inline_equation"},{"bbox":[331.6390686035156,437.292236328125,558.4277954101562,449.29718017578125],"content":"configuration may arise in the presence of a stretching ve-","score":1,"type":"text"}]},{"bbox":[303,448.251220703125,558,460.25616455078125],"spans":[{"bbox":[303.30706787109375,448.251220703125,558.4292602539062,460.25616455078125],"content":"locity field, as it would be the case of the tidal flow into the grav-","score":1,"type":"text"}]},{"bbox":[303,459.210205078125,558,471.21514892578125],"spans":[{"bbox":[303.30706787109375,459.210205078125,558.42919921875,471.21514892578125],"content":"itational well of a strongly self-gravitating cloud. 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Therefore, equation","score":1,"type":"text"}]},{"bbox":[303,492,558,504.09112548828125],"spans":[{"bbox":[303.30706787109375,492.086181640625,494.9374694824219,504.09112548828125],"content":"(7) for a positive velocity gradient implies that","score":1,"type":"text"},{"bbox":[494.9374694824219,492.086181640625,498.3570556640625,503.9815368652344],"content":" ","score":1,"type":"text"},{"bbox":[497,492,527,504],"content":"d B_{y}/d t","score":0.91,"type":"inline_equation"},{"bbox":[525.9519653320312,492.086181640625,558.4227294921875,504.09112548828125],"content":" has the","score":1,"type":"text"}]},{"bbox":[303,503,558,515.0501098632812],"spans":[{"bbox":[303.30706787109375,503.045166015625,367.4561767578125,515.0501098632812],"content":"opposite sign to","score":1,"type":"text"},{"bbox":[369,503,380,515],"content":"B_{y}","score":0.88,"type":"inline_equation"},{"bbox":[380.4080505371094,503.045166015625,558.4298095703125,515.0501098632812],"content":", straightening the field lines. Thus, we sug-","score":1,"type":"text"}]},{"bbox":[303,514.004150390625,558,526.0090942382812],"spans":[{"bbox":[303.30706787109375,514.004150390625,558.4290771484375,526.0090942382812],"content":"gest that the induction equation in the presence of a compressive","score":1,"type":"text"}]},{"bbox":[303,524.963134765625,558,536.9680786132812],"spans":[{"bbox":[303.30706787109375,524.963134765625,461.3536071777344,536.9680786132812],"content":"or stretching velocity field leads to the","score":1,"type":"text"},{"bbox":[461.3536071777344,526.390380859375,464.7560729980469,536.35302734375],"content":" ","score":1,"type":"text"},{"bbox":[464,525,509,536],"content":"\\phi\\,=\\,0,90^{\\circ}","score":0.91,"type":"inline_equation"},{"bbox":[511.9290771484375,524.963134765625,558.4246215820312,536.9680786132812],"content":"equilibrium","score":1,"type":"text"}]},{"bbox":[303,535.922119140625,558,547.9270629882812],"spans":[{"bbox":[303.30706787109375,535.922119140625,558.42919921875,547.9270629882812],"content":"configurations found by Soler & Hennebelle (2017), justifying","score":1,"type":"text"}]},{"bbox":[303,546.881103515625,558,558.8860473632812],"spans":[{"bbox":[303.30706787109375,546.881103515625,558.42919921875,558.8860473632812],"content":"their speculation that they may be attractors. 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However, our simulations include strong","score":1,"type":"text"}]},{"bbox":[303,727.0520629882812,558,739.0570068359375],"spans":[{"bbox":[303.3070068359375,727.0520629882812,558.4290161132812,739.0570068359375],"content":"cooling leading to thermal instability, which produces a much","score":1,"type":"text"}]},{"bbox":[303,738.0111083984375,558,750.0160522460938],"spans":[{"bbox":[303.3070068359375,738.0111083984375,558.4292602539062,750.0160522460938],"content":"stronger compression of the condensed layer and a much thin-","score":1,"type":"text"}]},{"bbox":[303,748.9700927734375,558,760.9750366210938],"spans":[{"bbox":[303.3070068359375,748.9700927734375,558.4292602539062,760.9750366210938],"content":"ner slab dimension, even for moderate Mach numbers (Vázquez-","score":1,"type":"text"}]}],"type":"text"}]},{"discarded_blocks":[{"bbox":[173,34,421,43],"lines":[{"bbox":[174.968994140625,32.58107376098633,420.3074951171875,43.38558578491211],"spans":[{"bbox":[174.968994140625,32.58107376098633,420.3074951171875,43.38558578491211],"content":"Granda-Muñoz et al.: Magnetic field alignment in interstellar clouds","score":1,"type":"text"}]}],"type":"discarded"},{"bbox":[454,770,559,780],"lines":[{"bbox":[455.19500732421875,769.81591796875,558.4251708984375,780.6204223632812],"spans":[{"bbox":[455.19500732421875,769.81591796875,558.4251708984375,780.6204223632812],"content":"Article number, page 7 of 11","score":1,"type":"text"}]}],"type":"discarded"}],"page_idx":6,"page_size":[595.2760009765625,841.8900146484375],"preproc_blocks":[{"bbox":[34,53,560,421],"blocks":[{"bbox":[90,53,504,364],"lines":[{"bbox":[90,53,504,364],"spans":[{"bbox":[90,53,504,364],"image_path":"aca9ca0eba0cfc506c1ed152a99dde59fcdfdff8ca6469b58b582da21fa829cf.jpg","score":0.9999658465385437,"type":"image"}]}],"type":"image_body"},{"bbox":[34,369,560,421],"lines":[{"bbox":[36.849998474121094,369.34027099609375,558.4263305664062,381.0055847167969],"spans":[{"bbox":[36.849998474121094,369.34027099609375,61.19377517700195,381.0055847167969],"content":"Fig. 4.","score":1,"type":"text"},{"bbox":[61.19377517700195,369.6630859375,558.4263305664062,380.46759033203125],"content":" Regions used to compute the HRO diagram and the shape parameter shown in Figure 3. 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It can be seen that, for the four density","score":1,"type":"text"}]},{"bbox":[36.850006103515625,399.5511169433594,558.4254150390625,410.3556213378906],"spans":[{"bbox":[36.850006103515625,399.5511169433594,558.4254150390625,410.3556213378906],"content":"intervals shown here, the magnetic field is noticeably parallel to the density structures. However, the magnetic field shows a deviation from this","score":1,"type":"text"}]},{"bbox":[36.850006103515625,409.5141296386719,528.2625122070312,420.3186340332031],"spans":[{"bbox":[36.850006103515625,409.5141296386719,528.2625122070312,420.3186340332031],"content":"trend for the highest density interval in the bottom right panel. We provide animations showing these regions as complementary material.","score":1,"type":"text"}]}],"type":"image_caption"}],"type":"image"},{"bbox":[34,434,294,594],"blocks":[{"bbox":[39,434,285,556],"lines":[{"bbox":[39,434,285,556],"spans":[{"bbox":[39,434,285,556],"image_path":"20309197b63052a64026f18a145ddb4f27a29b93ae7e58f1c22554a3457647fe.jpg","score":0.999991774559021,"type":"image"}]}],"type":"image_body"},{"bbox":[34,562,294,594],"lines":[{"bbox":[36.849998474121094,561.5473022460938,291.9652099609375,573.2125854492188],"spans":[{"bbox":[36.849998474121094,561.5473022460938,61.66899490356445,573.2125854492188],"content":"Fig. 5.","score":1,"type":"text"},{"bbox":[61.66899490356445,561.8700561523438,291.9652099609375,572.674560546875],"content":" Initial line bending model. The magnetic field is represented","score":1,"type":"text"}]},{"bbox":[36.85000228881836,571.8330688476562,291.970947265625,582.6375732421875],"spans":[{"bbox":[36.85000228881836,571.8330688476562,291.970947265625,582.6375732421875],"content":"by the green line, while the velocity field is represented by the black","score":1,"type":"text"}]},{"bbox":[36.85000228881836,581.7960815429688,63.2650146484375,592.6005859375],"spans":[{"bbox":[36.85000228881836,581.7960815429688,63.2650146484375,592.6005859375],"content":"arrows.","score":1,"type":"text"}]}],"type":"image_caption"}],"type":"image"},{"bbox":[36,612.403564453125,291,690.1625366210938],"lines":[{"bbox":[36,612.403564453125,291,624.4085083007812],"spans":[{"bbox":[36.85000228881836,612.403564453125,184.93408203125,624.4085083007812],"content":"Semadeni et al. 1996). So, it is not di","score":1,"type":"text"},{"bbox":[184.9320068359375,614.056884765625,193.17108154296875,624.0194702148438],"content":"ffi","score":1,"type":"text"},{"bbox":[193.17100524902344,612.403564453125,291.9700927734375,624.4085083007812],"content":"cult to fulfill the require-","score":1,"type":"text"}]},{"bbox":[36,623.3626098632812,291,635.3675537109375],"spans":[{"bbox":[36.850006103515625,623.3626098632812,218.0796661376953,635.3675537109375],"content":"ment for the development of the NTSI at the","score":1,"type":"text"},{"bbox":[218.0796661376953,623.3626098632812,263.1861267089844,635.2579345703125],"content":" condensed","score":1,"type":"text"},{"bbox":[263.1860046386719,623.3626098632812,291.96795654296875,635.3675537109375],"content":", rather","score":1,"type":"text"}]},{"bbox":[36,634.3215942382812,291,646.3265380859375],"spans":[{"bbox":[36.850006103515625,634.3215942382812,291.97222900390625,646.3265380859375],"content":"than the shocked, layer (Hueckstaedt 2003), as demonstrated by","score":1,"type":"text"}]},{"bbox":[36,645.2805786132812,291,657.2855224609375],"spans":[{"bbox":[36.850006103515625,645.2805786132812,291.9722595214844,657.2855224609375],"content":"the growth of the bending mode perturbation (the increase in","score":1,"type":"text"}]},{"bbox":[36,656.2396240234375,291,668.2445678710938],"spans":[{"bbox":[36.850006103515625,656.2396240234375,291.9722595214844,668.2445678710938],"content":"the curvature) for the dense layer in our 2D simulation. This","score":1,"type":"text"}]},{"bbox":[36,667.1986083984375,291,679.2035522460938],"spans":[{"bbox":[36.850006103515625,667.1986083984375,291.97222900390625,679.2035522460938],"content":"means that NTSI can be triggered by not-so-strong shocks in","score":1,"type":"text"}]},{"bbox":[36,678.1575927734375,138.677734375,690.1625366210938],"spans":[{"bbox":[36.850006103515625,678.1575927734375,138.677734375,690.1625366210938],"content":"the strongly cooling case.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[36,707,273,730],"lines":[{"bbox":[36.850006103515625,708.120361328125,272.42156982421875,719.83740234375],"spans":[{"bbox":[36.850006103515625,708.120361328125,272.42156982421875,719.83740234375],"content":"5.4. The effect of the magnetic field on the NTSI and the","score":1,"type":"text"}]},{"bbox":[55.95500564575195,719.0794067382812,105.30291748046875,730.7964477539062],"spans":[{"bbox":[55.95500564575195,719.0794067382812,105.30291748046875,730.7964477539062],"content":"shear strain","score":1,"type":"text"}]}],"type":"title"},{"bbox":[36,738.0115966796875,291,760.9755249023438],"lines":[{"bbox":[36,738.0115966796875,291,750.0165405273438],"spans":[{"bbox":[36.850006103515625,738.0115966796875,291.9722595214844,750.0165405273438],"content":"The NTSI is one of the possible mechanisms yielding the shear","score":1,"type":"text"}]},{"bbox":[36,748.9705810546875,291,760.9755249023438],"spans":[{"bbox":[36.850006103515625,748.9705810546875,291.9721984863281,760.9755249023438],"content":"strain proposed by Hennebelle (2013) to be responsible for the","score":1,"type":"text"}]},{"bbox":[303,438.42962646484375,558,450.4345703125],"spans":[{"bbox":[303.3070068359375,438.42962646484375,558.42919921875,450.4345703125],"content":"elongation of filamentary CACs and the alignment of these struc-","score":1,"type":"text"}]},{"bbox":[303,449.38861083984375,558,461.3935546875],"spans":[{"bbox":[303.3070068359375,449.38861083984375,558.42919921875,461.3935546875],"content":"tures with the local magnetic field, since it produces the momen-","score":1,"type":"text"}]},{"bbox":[303,460.34759521484375,558,472.3525390625],"spans":[{"bbox":[303.3070068359375,460.34759521484375,558.4291381835938,472.3525390625],"content":"tum transport from the original inflow direction to that parallel","score":1,"type":"text"}]},{"bbox":[303,471.30657958984375,558,483.3115234375],"spans":[{"bbox":[303.3070068359375,471.30657958984375,558.4290161132812,483.3115234375],"content":"to the dense layer in the regions around the nodes, as can be","score":1,"type":"text"}]},{"bbox":[303,482.26556396484375,558,494.2705078125],"spans":[{"bbox":[303.3070068359375,482.26556396484375,558.4292602539062,494.2705078125],"content":"seen in Figure 7. However, Heitsch et al. (2007) found that when","score":1,"type":"text"}]},{"bbox":[303,493.22454833984375,558,505.2294921875],"spans":[{"bbox":[303.3070068359375,493.22454833984375,558.4292602539062,505.2294921875],"content":"the magnetic field is aligned with the inflow, it tends to weaken","score":1,"type":"text"}]},{"bbox":[303,504.18353271484375,558,516.1884765625],"spans":[{"bbox":[303.3070068359375,504.18353271484375,558.4293212890625,516.1884765625],"content":"or even suppress the NTSI due to the magnetic tension coun-","score":1,"type":"text"}]},{"bbox":[303,515.1425170898438,558,527.1474609375],"spans":[{"bbox":[303.3070068359375,515.1425170898438,558.42919921875,527.1474609375],"content":"teracting the transverse momentum transport. Nevertheless, the","score":1,"type":"text"}]},{"bbox":[303,526.1015014648438,558,538.1064453125],"spans":[{"bbox":[303.3070068359375,526.1015014648438,325.44390869140625,538.1064453125],"content":"NTSI","score":1,"type":"text"},{"bbox":[325.44390869140625,526.1015014648438,342.78399658203125,537.996826171875],"content":" can","score":1,"type":"text"},{"bbox":[342.78399658203125,526.1015014648438,558.4205322265625,538.1064453125],"content":" contribute to the change of direction of the magnetic","score":1,"type":"text"}]},{"bbox":[303,537.0604858398438,558,549.0654296875],"spans":[{"bbox":[303.3070068359375,537.0604858398438,558.4291381835938,549.0654296875],"content":"field if the flow surrounding the dense layer, remains at least","score":1,"type":"text"}]},{"bbox":[303,548.0184936523438,558,560.0234375],"spans":[{"bbox":[303.3070068359375,548.0184936523438,426.56427001953125,560.0234375],"content":"transalfvénic, so that it has su","score":1,"type":"text"},{"bbox":[426.56298828125,549.6718139648438,434.80206298828125,559.6343994140625],"content":"ffi","score":1,"type":"text"},{"bbox":[434.802001953125,548.0184936523438,558.4279174804688,560.0234375],"content":"cient energy to bend the field.","score":1,"type":"text"}]},{"bbox":[303,558.9774780273438,558,570.982421875],"spans":[{"bbox":[303.3070068359375,558.9774780273438,558.4292602539062,570.982421875],"content":"This condition is indeed satisfied by the flow between the shock","score":1,"type":"text"}]},{"bbox":[303,569.9364624023438,558,581.94140625],"spans":[{"bbox":[303.3070068359375,569.9364624023438,558.4290771484375,581.94140625],"content":"and the condensation front, as can be seen for the 2D simulation","score":1,"type":"text"}]},{"bbox":[303,580.8954467773438,558,592.900390625],"spans":[{"bbox":[303.3070068359375,580.8954467773438,558.4290161132812,592.900390625],"content":"in both panels of Figure 7. Note, incidentally, that the flow inside","score":1,"type":"text"}]},{"bbox":[303,591.8544921875,462.6687316894531,603.8594360351562],"spans":[{"bbox":[303.3070068359375,591.8544921875,462.6687316894531,603.8594360351562],"content":"the dense layer is generally subalfvénic.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[303,438.42962646484375,558,603.8594360351562],"lines":[],"lines_deleted":true,"type":"text"},{"bbox":[303,606.5044555664062,558,760.9754028320312],"lines":[{"bbox":[318.2510070800781,606.5044555664062,558,618.5093994140625],"spans":[{"bbox":[318.2510070800781,606.5044555664062,558.4293212890625,618.5093994140625],"content":"Another source of shear strain that does not require the NTSI","score":1,"type":"text"}]},{"bbox":[303,617.4634399414062,558,629.4683837890625],"spans":[{"bbox":[303.3070068359375,617.4634399414062,558.42919921875,629.4683837890625],"content":"is observed in our 3D simulation, which does not include an ini-","score":1,"type":"text"}]},{"bbox":[303,628.4224853515625,558,640.4274291992188],"spans":[{"bbox":[303.3070068359375,628.4224853515625,558.4291381835938,640.4274291992188],"content":"tial bending-mode perturbation to the locus of the collision front.","score":1,"type":"text"}]},{"bbox":[303,639.3814697265625,558,651.3864135742188],"spans":[{"bbox":[303.3070068359375,639.3814697265625,558.4292602539062,651.3864135742188],"content":"This arises later in the evolution, when the magnetic field lines","score":1,"type":"text"}]},{"bbox":[303,650.3404541015625,558,662.3453979492188],"spans":[{"bbox":[303.3070068359375,650.3404541015625,558.4293212890625,662.3453979492188],"content":"have already been dragged and bent by the compressive velocity","score":1,"type":"text"}]},{"bbox":[303,661.2994384765625,558,673.3043823242188],"spans":[{"bbox":[303.3070068359375,661.2994384765625,558.42919921875,673.3043823242188],"content":"field. At this time, the transalfvénic condition of the post-shock","score":1,"type":"text"}]},{"bbox":[303,672.2574462890625,558,684.2623901367188],"spans":[{"bbox":[303.3070068359375,672.2574462890625,558.4291381835938,684.2623901367188],"content":"flow allows the magnetic field to partially re-orient the gas flow","score":1,"type":"text"}]},{"bbox":[303,683.2164306640625,558,695.2213745117188],"spans":[{"bbox":[303.3070068359375,683.2164306640625,558.4293212890625,695.2213745117188],"content":"along them. Since the field lines have been oriented nearly par-","score":1,"type":"text"}]},{"bbox":[303,694.1754150390625,558,706.1803588867188],"spans":[{"bbox":[303.3070068359375,694.1754150390625,558.42919921875,706.1803588867188],"content":"allel to the dense layer by the compressive post-shock flow, the","score":1,"type":"text"}]},{"bbox":[303,705.1344604492188,558,717.139404296875],"spans":[{"bbox":[303.3070068359375,705.1344604492188,558.4292602539062,717.139404296875],"content":"velocity field is also oriented in a similar way, and in opposite","score":1,"type":"text"}]},{"bbox":[303,716.0934448242188,558,728.098388671875],"spans":[{"bbox":[303.3070068359375,716.0934448242188,558.4293212890625,728.098388671875],"content":"directions on each side of the dense layer, therefore adding a","score":1,"type":"text"}]},{"bbox":[303,727.0524291992188,558,739.057373046875],"spans":[{"bbox":[303.3070068359375,727.0524291992188,558.4293823242188,739.057373046875],"content":"strong shear component to the flow around the layer. 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How-","score":1,"type":"text"}]},{"bbox":[36,436.633544921875,291,448.63848876953125],"spans":[{"bbox":[36.8499755859375,436.633544921875,291.9722595214844,448.63848876953125],"content":"ever, the main physical processes responsible for the alignment","score":1,"type":"text"}]},{"bbox":[36,447.592529296875,291,459.59747314453125],"spans":[{"bbox":[36.8499755859375,447.592529296875,291.9722595214844,459.59747314453125],"content":"of magnetic field lines and density structures, MHD shocks, and","score":1,"type":"text"}]},{"bbox":[36,458.551513671875,291,470.55645751953125],"spans":[{"bbox":[36.8499755859375,458.551513671875,291.9722595214844,470.55645751953125],"content":"the NTSI, can be also present at the interfaces between interact-","score":1,"type":"text"}]},{"bbox":[36,469.510498046875,291,481.51544189453125],"spans":[{"bbox":[36.8499755859375,469.510498046875,150.64280700683594,481.51544189453125],"content":"ing wind-blown bubbles and","score":1,"type":"text"},{"bbox":[150.64097595214844,471.163818359375,153.3607635498047,481.1264343261719],"content":"/","score":1,"type":"text"},{"bbox":[153.36097717285156,469.510498046875,291.9706115722656,481.51544189453125],"content":"or supernova shells. Therefore, the","score":1,"type":"text"}]},{"bbox":[36,480.468505859375,291,492.47344970703125],"spans":[{"bbox":[36.8499755859375,480.468505859375,291.9721984863281,492.47344970703125],"content":"MHD shocks and the NTSI could also be the principal physi-","score":1,"type":"text"}]},{"bbox":[36,491.427490234375,291,503.43243408203125],"spans":[{"bbox":[36.8499755859375,491.427490234375,291.97222900390625,503.43243408203125],"content":"cal mechanisms behind the magnetic field alignment with fibers","score":1,"type":"text"}]},{"bbox":[36,502.386474609375,234.97616577148438,514.3914184570312],"spans":[{"bbox":[36.8499755859375,502.386474609375,234.97616577148438,514.3914184570312],"content":"found in this type of object by Clark et al. (2014).","score":1,"type":"text"}]}],"type":"text"},{"bbox":[36,534,182,545],"lines":[{"bbox":[36.8499755859375,532.9898681640625,182.31346130371094,546.006591796875],"spans":[{"bbox":[36.8499755859375,532.9898681640625,182.31346130371094,546.006591796875],"content":"6. Summary and Conclusions","score":1,"type":"text"}]}],"type":"title"},{"bbox":[36,551.219482421875,291,639.9373779296875],"lines":[{"bbox":[36,551.219482421875,291,563.2244262695312],"spans":[{"bbox":[36.8499755859375,551.219482421875,291.97222900390625,563.2244262695312],"content":"In this work, we have studied the physical mechanisms responsi-","score":1,"type":"text"}]},{"bbox":[36,562.178466796875,291,574.1834106445312],"spans":[{"bbox":[36.8499755859375,562.178466796875,291.97222900390625,574.1834106445312],"content":"ble for the observed alignment of magnetic field and cold atomic","score":1,"type":"text"}]},{"bbox":[36,573.137451171875,291,585.1423950195312],"spans":[{"bbox":[36.8499755859375,573.137451171875,291.9721984863281,585.1423950195312],"content":"gravitationally unbound density structures formed by the colli-","score":1,"type":"text"}]},{"bbox":[36,584.096435546875,291,596.1013793945312],"spans":[{"bbox":[36.8499755859375,584.096435546875,291.9722595214844,596.1013793945312],"content":"sion of converging warm atomic gas. We have tracked the evo-","score":1,"type":"text"}]},{"bbox":[36,595.055419921875,291,607.0603637695312],"spans":[{"bbox":[36.8499755859375,595.055419921875,291.9721984863281,607.0603637695312],"content":"lution of magnetic field lines in a three-dimensional simulation","score":1,"type":"text"}]},{"bbox":[36,606.0144653320312,291,618.0194091796875],"spans":[{"bbox":[36.8499755859375,606.0144653320312,291.9721374511719,618.0194091796875],"content":"having typical conditions of the warm ISM and found that they","score":1,"type":"text"}]},{"bbox":[36,616.9734497070312,291,628.9783935546875],"spans":[{"bbox":[36.8499755859375,616.9734497070312,291.97222900390625,628.9783935546875],"content":"become perpendicular to their original orientation and end up","score":1,"type":"text"}]},{"bbox":[36,627.9324340820312,161.37249755859375,639.9373779296875],"spans":[{"bbox":[36.8499755859375,627.9324340820312,161.37249755859375,639.9373779296875],"content":"aligned with density structures.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[36,639.136474609375,291,694.8667602539062],"lines":[{"bbox":[51,639.136474609375,291,651.1414184570312],"spans":[{"bbox":[51.793975830078125,639.136474609375,291.9723205566406,651.1414184570312],"content":"The process of the alignment of magnetic field lines with","score":1,"type":"text"}]},{"bbox":[36,650.095458984375,291,662.1004028320312],"spans":[{"bbox":[36.8499755859375,650.095458984375,122.99655151367188,662.1004028320312],"content":"the density structures","score":1,"type":"text"},{"bbox":[122.99655151367188,650.095458984375,226.50059509277344,661.9907836914062],"content":" starts at the shock fronts","score":1,"type":"text"},{"bbox":[226.50059509277344,650.095458984375,291.96734619140625,662.1004028320312],"content":" and takes place","score":1,"type":"text"}]},{"bbox":[36,661.053466796875,291,672.9487915039062],"spans":[{"bbox":[36.8499755859375,661.053466796875,291.9721984863281,672.9487915039062],"content":"in the cooling, thermally unstable gas, so that the magnetic field","score":1,"type":"text"}]},{"bbox":[36,672.012451171875,291,683.9077758789062],"spans":[{"bbox":[36.8499755859375,672.012451171875,291.97222900390625,683.9077758789062],"content":"already shows a preferred orientation when the flow forms CACs","score":1,"type":"text"}]},{"bbox":[36,682.971435546875,128.15719604492188,694.8667602539062],"spans":[{"bbox":[36.8499755859375,682.971435546875,128.15719604492188,694.8667602539062],"content":"at the condensed layer.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[36,694.1754150390625,291,760.9754028320312],"lines":[{"bbox":[51,694.1754150390625,291,706.1803588867188],"spans":[{"bbox":[51.793975830078125,694.1754150390625,291.9723205566406,706.1803588867188],"content":"At the position of the shocks, the magnetic field changes its","score":1,"type":"text"}]},{"bbox":[36,705.1343994140625,291,717.1393432617188],"spans":[{"bbox":[36.8499755859375,705.1343994140625,291.97216796875,717.1393432617188],"content":"direction due to the amplification of its component parallel to","score":1,"type":"text"}]},{"bbox":[36,716.0934448242188,291,728.098388671875],"spans":[{"bbox":[36.8499755859375,716.0934448242188,291.97216796875,728.098388671875],"content":"the front, which is produced by the velocity fluctuations in the","score":1,"type":"text"}]},{"bbox":[36,727.0524291992188,291,739.057373046875],"spans":[{"bbox":[36.8499755859375,727.0524291992188,291.97222900390625,739.057373046875],"content":"pre-shock region. This amplification occurs due to a fast MHD","score":1,"type":"text"}]},{"bbox":[36,738.0114135742188,291,750.016357421875],"spans":[{"bbox":[36.8499755859375,738.0114135742188,291.97222900390625,750.016357421875],"content":"shock that occurs when the upstream and downstream flows are","score":1,"type":"text"}]},{"bbox":[36,748.970458984375,168.5854034423828,760.9754028320312],"spans":[{"bbox":[36.8499755859375,748.970458984375,168.5854034423828,760.9754028320312],"content":"super– and sub-fast, respectively.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[303,56.56640625,558,167.2012176513672],"lines":[{"bbox":[318,56.56640625,558,68.57134246826172],"spans":[{"bbox":[318.2509765625,56.56640625,558.4293212890625,68.57134246826172],"content":"Behind the shock front, the compressive downstream veloc-","score":1,"type":"text"}]},{"bbox":[303,67.525390625,558,79.53032684326172],"spans":[{"bbox":[303.3069763183594,67.525390625,558.4292602539062,79.53032684326172],"content":"ity field further amplifies the magnetic field component parallel","score":1,"type":"text"}]},{"bbox":[303,78.484375,558,90.48931121826172],"spans":[{"bbox":[303.3069763183594,78.484375,558.4290161132812,90.48931121826172],"content":"to the shock front, increasing the curvature of the lines in this","score":1,"type":"text"}]},{"bbox":[303,89.443359375,558,101.44829559326172],"spans":[{"bbox":[303.3069763183594,89.443359375,558.4291381835938,101.44829559326172],"content":"region, and causing them to become increasingly parallel to the","score":1,"type":"text"}]},{"bbox":[303,100.40234375,558,112.40727996826172],"spans":[{"bbox":[303.3069763183594,100.40234375,558.4291381835938,112.40727996826172],"content":"condensed layer produced by the thermal instability. The ampli-","score":1,"type":"text"}]},{"bbox":[303,111.361328125,558,123.36626434326172],"spans":[{"bbox":[303.3069763183594,111.361328125,558.4292602539062,123.36626434326172],"content":"fication of the fluctuation by a compressive velocity gradient can","score":1,"type":"text"}]},{"bbox":[303,122.3203125,558,134.3252410888672],"spans":[{"bbox":[303.3069763183594,122.3203125,558.4290771484375,134.3252410888672],"content":"be understood through an analysis of the induction equation for","score":1,"type":"text"}]},{"bbox":[303,133.279296875,558,145.2842254638672],"spans":[{"bbox":[303.3069763183594,133.279296875,558.4292602539062,145.2842254638672],"content":"planar geometry (eq. [7]), which shows that the change in the","score":1,"type":"text"}]},{"bbox":[303,144.2373046875,558,156.2422332763672],"spans":[{"bbox":[303.3069763183594,144.2373046875,558.4293212890625,156.2422332763672],"content":"fluctuating field component has the same sign as the fluctuation,","score":1,"type":"text"}]},{"bbox":[303,155.1962890625,357.55328369140625,167.2012176513672],"spans":[{"bbox":[303.3069763183594,155.1962890625,357.55328369140625,167.2012176513672],"content":"amplifying it.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[303,166.1552734375,558,265.83209228515625],"lines":[{"bbox":[318,166.1552734375,558,178.1602020263672],"spans":[{"bbox":[318.2509765625,166.1552734375,558.429443359375,178.1602020263672],"content":"From the same equation, we concluded that a stretching ve-","score":1,"type":"text"}]},{"bbox":[303,177.1142578125,558,189.1191864013672],"spans":[{"bbox":[303.3069763183594,177.1142578125,392.9504089355469,189.1191864013672],"content":"locity gradient causes","score":1,"type":"text"},{"bbox":[392.9504089355469,177.1142578125,431.9690246582031,189.0095977783203],"content":" damping","score":1,"type":"text"},{"bbox":[431.9690246582031,177.1142578125,558.4298706054688,189.1191864013672],"content":" of the fluctuating component,","score":1,"type":"text"}]},{"bbox":[303,188.0732421875,558,200.0781707763672],"spans":[{"bbox":[303.3070068359375,188.0732421875,558.4291381835938,200.0781707763672],"content":"leading to a straightening of the field lines, thus orienting them","score":1,"type":"text"}]},{"bbox":[303,199.0322265625,558,211.0371551513672],"spans":[{"bbox":[303.3070068359375,199.0322265625,359.75506591796875,210.9275665283203],"content":"perpendicular","score":1,"type":"text"},{"bbox":[359.75506591796875,199.0322265625,558.4254760742188,211.0371551513672],"content":" to the density structures. We speculate that this is","score":1,"type":"text"}]},{"bbox":[303,209.9912109375,558,221.9961395263672],"spans":[{"bbox":[303.3070068359375,209.9912109375,558.42919921875,221.9961395263672],"content":"the mechanism occurring during the growth of self-gravitating","score":1,"type":"text"}]},{"bbox":[303,220.9501953125,558,232.9551239013672],"spans":[{"bbox":[303.3070068359375,220.9501953125,408.6913757324219,232.9551239013672],"content":"structures, where the flow","score":1,"type":"text"},{"bbox":[408.6913757324219,220.9501953125,457.3052673339844,232.8455352783203],"content":" accelerates","score":1,"type":"text"},{"bbox":[457.3052673339844,220.9501953125,558.4212646484375,232.9551239013672],"content":" inwards, thus producing","score":1,"type":"text"}]},{"bbox":[303,231.9091796875,558,243.9141082763672],"spans":[{"bbox":[303.3070068359375,231.9091796875,558.4291381835938,243.9141082763672],"content":"a tidal stretching velocity pattern, thus being a possible expla-","score":1,"type":"text"}]},{"bbox":[303,242.8681640625,558,254.8730926513672],"spans":[{"bbox":[303.3070068359375,242.8681640625,558.4290771484375,254.8730926513672],"content":"nation for the perpendicular orientation of the field lines around","score":1,"type":"text"}]},{"bbox":[303,253.8271484375,472.45196533203125,265.83209228515625],"spans":[{"bbox":[303.3070068359375,253.8271484375,472.45196533203125,265.83209228515625],"content":"self-gravitating molecular cloud filaments.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[303,264.78515625,558,353.50299072265625],"lines":[{"bbox":[318,264.78515625,558,276.79010009765625],"spans":[{"bbox":[318.2510070800781,264.78515625,462.8480529785156,276.79010009765625],"content":"In conclusion, we have found that a","score":1,"type":"text"},{"bbox":[462.8480529785156,264.78515625,495.1838073730469,276.6805114746094],"content":" settling","score":1,"type":"text"},{"bbox":[495.1838073730469,264.78515625,558.4208984375,276.79010009765625],"content":" (i.e., decelerat-","score":1,"type":"text"}]},{"bbox":[303,275.744140625,558,287.74908447265625],"spans":[{"bbox":[303.3070068359375,275.744140625,558.42919921875,287.74908447265625],"content":"ing) flow, such as that occurring due to the condensation of the","score":1,"type":"text"}]},{"bbox":[303,286.703125,558,298.70806884765625],"spans":[{"bbox":[303.3070068359375,286.703125,558.42919921875,298.70806884765625],"content":"gas by thermal instability orients the lines parallel to the density","score":1,"type":"text"}]},{"bbox":[303,297.662109375,558,309.66705322265625],"spans":[{"bbox":[303.3070068359375,297.662109375,378.3054504394531,309.66705322265625],"content":"structures, while a","score":1,"type":"text"},{"bbox":[378.3054504394531,297.662109375,421.25030517578125,309.5574645996094],"content":" stretching","score":1,"type":"text"},{"bbox":[421.25030517578125,297.662109375,558.4276123046875,309.66705322265625],"content":" (accelerating) one, such as infall","score":1,"type":"text"}]},{"bbox":[303,308.62109375,558,320.62603759765625],"spans":[{"bbox":[303.3070068359375,308.62109375,558.42919921875,320.62603759765625],"content":"into a potential well, orients the field lines perpendicular to the","score":1,"type":"text"}]},{"bbox":[303,319.580078125,558,331.58502197265625],"spans":[{"bbox":[303.3070068359375,319.580078125,558.4292602539062,331.58502197265625],"content":"density structures. This may be the physical mechanism behind","score":1,"type":"text"}]},{"bbox":[303,330.5390625,558,342.54400634765625],"spans":[{"bbox":[303.3070068359375,330.5390625,558.42919921875,342.54400634765625],"content":"the stationarity of these configurations found by Soler & Hen-","score":1,"type":"text"}]},{"bbox":[303,341.498046875,363.62054443359375,353.50299072265625],"spans":[{"bbox":[303.3070068359375,341.498046875,363.62054443359375,353.50299072265625],"content":"nebelle (2017).","score":1,"type":"text"}]}],"type":"text"},{"bbox":[303,352.45703125,558,397.33795166015625],"lines":[{"bbox":[318,352.45703125,558,364.46197509765625],"spans":[{"bbox":[318.2510070800781,352.45703125,558.4293212890625,364.46197509765625],"content":"Finally, we also found that, under typical conditions of the","score":1,"type":"text"}]},{"bbox":[303,363.416015625,558,375.42095947265625],"spans":[{"bbox":[303.3070068359375,363.416015625,558.4293823242188,375.42095947265625],"content":"ISM, the flow upstream from the shock front is superalfvénic","score":1,"type":"text"}]},{"bbox":[303,374.3740234375,558,386.37896728515625],"spans":[{"bbox":[303.3070068359375,374.3740234375,558.4293823242188,386.37896728515625],"content":"and becomes transalfvénic downstream. This allows the velocity","score":1,"type":"text"}]},{"bbox":[303,385.3330078125,487.8741455078125,397.33795166015625],"spans":[{"bbox":[303.3070068359375,385.3330078125,487.8741455078125,397.33795166015625],"content":"field to bend and drag the magnetic field lines.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[303,402.0290832519531,558,464.89312744140625],"lines":[{"bbox":[303,402.0290832519531,558,411.633056640625],"spans":[{"bbox":[303.3070068359375,402.0290832519531,366.1512756347656,411.5453796386719],"content":"Acknowledgements.","score":1,"type":"text"},{"bbox":[366.1512756347656,402.0290832519531,558.4215698242188,411.633056640625],"content":" We are grateful to Susan Clark and Laura Fissel for use-","score":1,"type":"text"}]},{"bbox":[303,410.90509033203125,558,420.5090637207031],"spans":[{"bbox":[303.3070068359375,410.90509033203125,558.4219970703125,420.5090637207031],"content":"ful comments and suggestions. 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In these simulations, we follow the evolution","score":1,"type":"text"}]},{"bbox":[59,338.4340515136719,389.7962341308594,349.2385559082031],"spans":[{"bbox":[59.52794647216797,338.4340515136719,389.7962341308594,349.2385559082031],"content":"of magnetic field lines, identify and elucidate the physical processes causing their evolution.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[59,348.39605712890625,535,478.752685546875],"lines":[{"bbox":[59,348.39605712890625,535,359.2005615234375],"spans":[{"bbox":[59.52794647216797,348.5633544921875,90.16719818115234,359.108642578125],"content":"Results.","score":1,"type":"text"},{"bbox":[90.16719818115234,348.39605712890625,535.7520141601562,359.2005615234375],"content":" The collision produces a fast MHD shock, and a condensation front roughly one cooling length behind it, on each side","score":1,"type":"text"}]},{"bbox":[59,358.35906982421875,535,369.16357421875],"spans":[{"bbox":[59.527950286865234,358.35906982421875,535.7512817382812,369.16357421875],"content":"of the collision front. A cold dense layer forms behind the condensation front, onto which the gas settles, decelerating smoothly.","score":1,"type":"text"}]},{"bbox":[59,368.32208251953125,535,379.1265869140625],"spans":[{"bbox":[59.527950286865234,368.32208251953125,535.7512817382812,379.1265869140625],"content":"We find that the magnetic field lines, initially oriented parallel to the flow direction, are perturbed by the fast MHD shock, across","score":1,"type":"text"}]},{"bbox":[59,378.2840881347656,535,389.0885925292969],"spans":[{"bbox":[59.527950286865234,378.2840881347656,535.751220703125,389.0885925292969],"content":"which the magnetic field fluctuations parallel to the shock front are amplified. The downstream perturbations of the magnetic field","score":1,"type":"text"}]},{"bbox":[59,388.2471008300781,535,399.0516052246094],"spans":[{"bbox":[59.527950286865234,388.2471008300781,180.19773864746094,399.0516052246094],"content":"lines are further amplified by the","score":1,"type":"text"},{"bbox":[180.19773864746094,388.2471008300781,227.1071014404297,398.9529724121094],"content":" compressive","score":1,"type":"text"},{"bbox":[227.1071014404297,388.2471008300781,535.7522583007812,399.0516052246094],"content":" downstream velocity gradient between the shock and the condensation front caused","score":1,"type":"text"}]},{"bbox":[59,398.2101135253906,535,409.0146179199219],"spans":[{"bbox":[59.5279541015625,398.2101135253906,535.751220703125,409.0146179199219],"content":"by the settlement of the gas onto the dense layer. This mechanism causes the magnetic field to become increasingly parallel to the","score":1,"type":"text"}]},{"bbox":[59,408.172119140625,535,418.97662353515625],"spans":[{"bbox":[59.5279541015625,408.172119140625,535.7513427734375,418.97662353515625],"content":"dense layer, and the development of a shear flow around the latter. Furthermore, the bending-mode perturbations on the dense layer","score":1,"type":"text"}]},{"bbox":[59,418.1351318359375,535,428.93963623046875],"spans":[{"bbox":[59.5279541015625,418.1351318359375,535.7510375976562,428.93963623046875],"content":"are amplified by the non-linear thin-shell instability (NTSI), stretching the density structures formed by the thermal instability, and","score":1,"type":"text"}]},{"bbox":[59,428.09814453125,535,438.90264892578125],"spans":[{"bbox":[59.5279541015625,428.09814453125,355.9569396972656,438.90264892578125],"content":"rendering them parallel to the bent field lines. By extension, we suggest that a tidal","score":1,"type":"text"},{"bbox":[355.9569396972656,428.09814453125,393.57122802734375,438.80401611328125],"content":" stretching","score":1,"type":"text"},{"bbox":[393.57122802734375,428.09814453125,535.7483520507812,438.90264892578125],"content":" velocity gradient such as that produced","score":1,"type":"text"}]},{"bbox":[59,438.0601501464844,535,448.8646545410156],"spans":[{"bbox":[59.5279541015625,438.0601501464844,535.7513427734375,448.8646545410156],"content":"in gas infalling into a self-gravitating structure must straighten the field lines along the accretion flow, orienting them perpendicular","score":1,"type":"text"}]},{"bbox":[59,448.0231628417969,535,458.8276672363281],"spans":[{"bbox":[59.5279541015625,448.0231628417969,535.7510986328125,458.8276672363281],"content":"to the density structures. We also find that the upstream superalfvénic regime transitions to a transalfvénic regime between the shock","score":1,"type":"text"}]},{"bbox":[59,457.98516845703125,535,468.7896728515625],"spans":[{"bbox":[59.5279541015625,457.98516845703125,535.7510375976562,468.7896728515625],"content":"and the condensation front, and then to a subalfvénic regime inside the condensations. Finally, in two-dimensional simulations with a","score":1,"type":"text"}]},{"bbox":[59,467.94818115234375,524.3818969726562,478.752685546875],"spans":[{"bbox":[59.5279541015625,467.94818115234375,524.3818969726562,478.752685546875],"content":"curved collision front, the presence of the magnetic field inhibits the generation of turbulence by the shear around the dense layer.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[59,477.91119384765625,535,498.6777038574219],"lines":[{"bbox":[59,477.91119384765625,535,488.7156982421875],"spans":[{"bbox":[59.5279541015625,478.0784912109375,108.1572265625,488.623779296875],"content":"Conclusions.","score":1,"type":"text"},{"bbox":[108.1572265625,477.91119384765625,535.7467651367188,488.7156982421875],"content":" Our results provide a feasible physical mechanism for the observed transition from parallel to perpendicular relative","score":1,"type":"text"}]},{"bbox":[59,487.8731994628906,529,498.6777038574219],"spans":[{"bbox":[59.5279541015625,487.8731994628906,528.9368286132812,498.6777038574219],"content":"orientation of the magnetic field and the density structures as the density structures become increasingly dominated by self-gravity.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[59,503.8141784667969,420.0631103515625,514.7141723632812],"lines":[{"bbox":[59,503.8141784667969,420.0631103515625,514.7141723632812],"spans":[{"bbox":[59.5279541015625,504.0155334472656,104.37522888183594,514.7141723632812],"content":"Key words.","score":1,"type":"text"},{"bbox":[104.37522888183594,503.8141784667969,420.0631103515625,514.61865234375],"content":" Magnetic fields – ISM: clouds –ISM: magnetic fields – ISM: kinematics and dynamics","score":1,"type":"text"}]}],"type":"text"},{"bbox":[38,537,109,550],"lines":[{"bbox":[36.849952697753906,538.0780639648438,109.05316162109375,551.0947875976562],"spans":[{"bbox":[36.849952697753906,538.0780639648438,109.05316162109375,551.0947875976562],"content":"1. Introduction","score":1,"type":"text"}]}],"type":"title"},{"bbox":[37,562.668701171875,291,760.9756469726562],"lines":[{"bbox":[37,562.668701171875,291,574.6736450195312],"spans":[{"bbox":[36.849952697753906,562.668701171875,291.97222900390625,574.6736450195312],"content":"Studying the role of magnetic fields in the formation and evo-","score":1,"type":"text"}]},{"bbox":[37,573.627685546875,291,585.6326293945312],"spans":[{"bbox":[36.849952697753906,573.627685546875,291.9721984863281,585.6326293945312],"content":"lution of atomic and molecular clouds (MCs) has been an im-","score":1,"type":"text"}]},{"bbox":[37,584.586669921875,291,596.5916137695312],"spans":[{"bbox":[36.849952697753906,584.586669921875,291.97216796875,596.5916137695312],"content":"portant research topic for both observational and theoretical as-","score":1,"type":"text"}]},{"bbox":[37,595.545654296875,291,607.5505981445312],"spans":[{"bbox":[36.849952697753906,595.545654296875,291.9721374511719,607.5505981445312],"content":"tronomy. Magnetic fields are thought to be an important ingre-","score":1,"type":"text"}]},{"bbox":[37,606.5046997070312,291,618.5096435546875],"spans":[{"bbox":[36.849952697753906,606.5046997070312,291.97216796875,618.5096435546875],"content":"dient in the dynamics of the ISM, providing a possible support","score":1,"type":"text"}]},{"bbox":[37,617.4636840820312,291,629.4686279296875],"spans":[{"bbox":[36.849952697753906,617.4636840820312,291.97222900390625,629.4686279296875],"content":"mechanism against gravitational collapse, and guiding the gas","score":1,"type":"text"}]},{"bbox":[37,628.4226684570312,291,640.4276123046875],"spans":[{"bbox":[36.849952697753906,628.4226684570312,291.9721984863281,640.4276123046875],"content":"flow in the surroundings of filamentary structures, among many","score":1,"type":"text"}]},{"bbox":[37,639.3817138671875,291,651.3866577148438],"spans":[{"bbox":[36.849952697753906,639.3817138671875,65.88097381591797,651.3866577148438],"content":"other e","score":1,"type":"text"},{"bbox":[65.87995147705078,641.0350341796875,71.85751342773438,650.9976196289062],"content":"ff","score":1,"type":"text"},{"bbox":[71.85694885253906,639.3817138671875,291.9705810546875,651.3866577148438],"content":"ects. 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For example, Clark et al.","score":1,"type":"text"}]},{"bbox":[37,672.2586669921875,291,684.2636108398438],"spans":[{"bbox":[36.84994888305664,672.2586669921875,291.97222900390625,684.2636108398438],"content":"(2015) found that the plane of the sky magnetic field, measured","score":1,"type":"text"}]},{"bbox":[37,683.2166748046875,291,695.2216186523438],"spans":[{"bbox":[36.84994888305664,683.2166748046875,291.9721984863281,695.2216186523438],"content":"using polarized thermal dust emission, is aligned with atomic","score":1,"type":"text"}]},{"bbox":[37,694.1756591796875,291,706.1806030273438],"spans":[{"bbox":[36.84994888305664,694.1756591796875,291.97222900390625,706.1806030273438],"content":"hydrogen structures detected with HI emission and Clark et al.","score":1,"type":"text"}]},{"bbox":[37,705.1346435546875,291,717.1395874023438],"spans":[{"bbox":[36.84994888305664,705.1346435546875,234.73712158203125,717.1395874023438],"content":"(2014) also observed a similar alignment in HI","score":1,"type":"text"},{"bbox":[234.73712158203125,705.1346435546875,260.9491882324219,717.0299682617188],"content":" fibers","score":1,"type":"text"},{"bbox":[260.9489440917969,705.1346435546875,291.97247314453125,717.1395874023438],"content":", which","score":1,"type":"text"}]},{"bbox":[37,716.0936889648438,291,728.0986328125],"spans":[{"bbox":[36.849945068359375,716.0936889648438,291.9721984863281,728.0986328125],"content":"are thin long dense structures identified in HI emission using","score":1,"type":"text"}]},{"bbox":[37,727.0526733398438,291,739.0576171875],"spans":[{"bbox":[36.849945068359375,727.0526733398438,291.9721374511719,739.0576171875],"content":"the Rolling Hough transform. In addition, Planck Collabora-","score":1,"type":"text"}]},{"bbox":[37,738.0116577148438,291,750.0166015625],"spans":[{"bbox":[36.849945068359375,738.0116577148438,291.9721374511719,750.0166015625],"content":"tion et al. (2016a) found that the plane of the sky magnetic","score":1,"type":"text"}]},{"bbox":[37,748.970703125,291,760.9756469726562],"spans":[{"bbox":[36.849945068359375,748.970703125,291.97222900390625,760.9756469726562],"content":"field, detected using polarized thermal dust emission, is aligned","score":1,"type":"text"}]},{"bbox":[303,538.7076416015625,558,550.7125854492188],"spans":[{"bbox":[303.30694580078125,538.7076416015625,558.42919921875,550.7125854492188],"content":"with molecular structures traced by dust, and Planck Collabo-","score":1,"type":"text"}]},{"bbox":[303,549.6666870117188,558,561.671630859375],"spans":[{"bbox":[303.30694580078125,549.6666870117188,558.4290161132812,561.671630859375],"content":"ration et al. (2016b) found that the relative orientation of the","score":1,"type":"text"}]},{"bbox":[303,560.6256713867188,558,572.630615234375],"spans":[{"bbox":[303.30694580078125,560.6256713867188,558.42919921875,572.630615234375],"content":"projected magnetic field and dust filaments changes from par-","score":1,"type":"text"}]},{"bbox":[303,571.5846557617188,558,583.589599609375],"spans":[{"bbox":[303.30694580078125,571.5846557617188,558.42919921875,583.589599609375],"content":"allel to perpendicular when sampling higher density regions in","score":1,"type":"text"}]},{"bbox":[303,582.5426635742188,558,594.547607421875],"spans":[{"bbox":[303.30694580078125,582.5426635742188,558.4292602539062,594.547607421875],"content":"nearby MCs. Skalidis et al. (2022) studied the role of the mag-","score":1,"type":"text"}]},{"bbox":[303,593,558,607.0015869140625],"spans":[{"bbox":[303.30694580078125,593.5016479492188,445.662353515625,605.506591796875],"content":"netic field in the transition between ","score":1,"type":"text"},{"bbox":[445,593,478,604],"content":"\\mathrm{HI}-\\mathrm{H}_{2}","score":0.87,"type":"inline_equation"},{"bbox":[477.6148376464844,593.5016479492188,558.4295043945312,607.0015869140625],"content":" using multiple trac-","score":1,"type":"text"}]},{"bbox":[303,604.460693359375,558,616.4656372070312],"spans":[{"bbox":[303.3069152832031,604.460693359375,558.4293212890625,616.4656372070312],"content":"ers to investigate the gas properties of Ursa Minor. 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These intervals comprise the densities of the post-shock","score":1,"type":"text"}]},{"bbox":[35,406,291,418.8902587890625],"spans":[{"bbox":[36.84999084472656,406.88531494140625,83.08641052246094,418.8902587890625],"content":"warm neutr","score":1,"type":"text"},{"bbox":[129,406,202,417],"content":"\\bar{(n\\in[3,10]\\ \\mathrm{cm}^{-3})}","score":0.9,"type":"inline_equation"},{"bbox":[200.50498962402344,406.88531494140625,291.9715881347656,418.8902587890625],"content":"), the low-density cold","score":1,"type":"text"}]},{"bbox":[35,417,291,429.8492431640625],"spans":[{"bbox":[36.84999084472656,417.84429931640625,81.05404663085938,429.8492431640625],"content":"neutral gas","score":1,"type":"text"},{"bbox":[83,417,183,429],"content":"(n\\,\\in\\,[10,3\\times10^{1}]\\;\\mathrm{cm}^{-3})","score":0.87,"type":"inline_equation"},{"bbox":[182.13999938964844,417.84429931640625,291.9676818847656,429.8492431640625],"content":"), the medium-density cold","score":1,"type":"text"}]},{"bbox":[82,428.80328369140625,291,440.8082275390625],"spans":[{"bbox":[82,429,178,439],"content":"(n\\in[3{\\times}10^{1},10^{2}]\\,\\mathrm{cm}^{-3})","score":0.84,"type":"inline_equation"},{"bbox":[175.00701904296875,428.80328369140625,291.9678955078125,440.8082275390625],"content":"), the high-density neutral gas","score":1,"type":"text"}]},{"bbox":[35,439,291,458.3724060058594],"spans":[{"bbox":[36,439,133,451],"content":"(n\\in[10^{2},3\\times10^{2}]\\,\\mathrm{cm}^{-3})","score":0.86,"type":"inline_equation"},{"bbox":[45.149322509765625,440.340087890625,53.25697708129883,458.3724060058594],"content":" ∈","score":1,"type":"text"},{"bbox":[154.26364135742188,439.76226806640625,291.9666442871094,451.7672119140625],"content":" the density range of the central re-","score":1,"type":"text"}]},{"bbox":[35,450.72125244140625,291,469.3313903808594],"spans":[{"bbox":[36.85002136230469,450.72125244140625,59.98318099975586,462.7261962890625],"content":"gion (","score":1,"type":"text"},{"bbox":[56,451,152,462],"content":"(n\\in[3{\\times}10^{2},10^{3}]\\,\\mathrm{cm}^{-3})","score":0.87,"type":"inline_equation"},{"bbox":[64.96131896972656,451.299072265625,73.0689697265625,469.3313903808594],"content":" ∈","score":1,"type":"text"},{"bbox":[84.89701843261719,451.299072265625,91.23323059082031,469.3313903808594],"content":"×","score":1,"type":"text"},{"bbox":[150.0530242919922,450.72125244140625,167.36802673339844,462.7261962890625],"content":"). 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It can be seen from this figure that the mag-","score":1,"type":"text"}]},{"bbox":[302,370.86822509765625,558,382.8731689453125],"spans":[{"bbox":[303.30694580078125,370.86822509765625,558.4290771484375,382.8731689453125],"content":"netic field (black arrows) tends to be parallel to the density struc-","score":1,"type":"text"}]},{"bbox":[302,381.82623291015625,558,393.8311767578125],"spans":[{"bbox":[303.30694580078125,381.82623291015625,558.4292602539062,393.8311767578125],"content":"tures for the four density intervals. However, for the highest den-","score":1,"type":"text"}]},{"bbox":[302,392.78521728515625,558,404.7901611328125],"spans":[{"bbox":[303.30694580078125,392.78521728515625,558.42919921875,404.7901611328125],"content":"sity interval, the magnetic field does not follow this general trend","score":1,"type":"text"}]},{"bbox":[302,403.74420166015625,558,415.7491455078125],"spans":[{"bbox":[303.30694580078125,403.74420166015625,558.4291381835938,415.7491455078125],"content":"in some regions, leading to the observed change in the shape pa-","score":1,"type":"text"}]},{"bbox":[302,414.70318603515625,335.6754455566406,426.7081298828125],"spans":[{"bbox":[303.30694580078125,414.70318603515625,335.6754455566406,426.7081298828125],"content":"rameter.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[303,456,453,468],"lines":[{"bbox":[303.30694580078125,456.5015869140625,453.48583984375,469.51824951171875],"spans":[{"bbox":[303.30694580078125,456.5015869140625,453.48583984375,469.51824951171875],"content":"4. Magnetic field line evolution","score":1,"type":"text"}]}],"type":"title"},{"bbox":[302,476.9701843261719,558,576.6460571289062],"lines":[{"bbox":[302,476.9701843261719,558,488.9751281738281],"spans":[{"bbox":[303.30694580078125,476.9701843261719,558.4291381835938,488.9751281738281],"content":"To understand the alignment of the magnetic field with CACs","score":1,"type":"text"}]},{"bbox":[302,487.92919921875,558,499.93414306640625],"spans":[{"bbox":[303.30694580078125,487.92919921875,558.42919921875,499.93414306640625],"content":"shown in the previous section, we followed the evolution of the","score":1,"type":"text"}]},{"bbox":[302,498.88720703125,558,510.89215087890625],"spans":[{"bbox":[303.30694580078125,498.88720703125,558.42919921875,510.89215087890625],"content":"magnetic field lines. The resulting configuration of the three-","score":1,"type":"text"}]},{"bbox":[302,509.84619140625,558,521.8511352539062],"spans":[{"bbox":[303.30694580078125,509.84619140625,558.42919921875,521.8511352539062],"content":"dimensional density structures and magnetic field lines of Re-","score":1,"type":"text"}]},{"bbox":[302,520.80517578125,558,532.8101196289062],"spans":[{"bbox":[303.30694580078125,520.80517578125,558.42919921875,532.8101196289062],"content":"gion R1 after 5 Myr of evolution is shown in Figure 2, where","score":1,"type":"text"}]},{"bbox":[302,531.76416015625,558,543.7691040039062],"spans":[{"bbox":[303.30694580078125,531.76416015625,558.4293823242188,543.7691040039062],"content":"we can see the shock fronts at each side of the central condensa-","score":1,"type":"text"}]},{"bbox":[302,542.72314453125,558,554.7280883789062],"spans":[{"bbox":[303.30694580078125,542.72314453125,558.4290161132812,554.7280883789062],"content":"tion region. The magnetic field lines start bending at these shock","score":1,"type":"text"}]},{"bbox":[302,553.68212890625,558,565.6870727539062],"spans":[{"bbox":[303.30694580078125,553.68212890625,558.42919921875,565.6870727539062],"content":"fronts along their way from the center of the computational do-","score":1,"type":"text"}]},{"bbox":[302,564.64111328125,326,576.6460571289062],"spans":[{"bbox":[303.30694580078125,564.64111328125,325.7228088378906,576.6460571289062],"content":"main.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[302,578.0841064453125,558,633.924072265625],"lines":[{"bbox":[318,578.0841064453125,558,590.0890502929688],"spans":[{"bbox":[318.2509460449219,578.0841064453125,558.4293823242188,590.0890502929688],"content":"As can be seen in the provided animation (Fig. 2), the mag-","score":1,"type":"text"}]},{"bbox":[302,589.0430908203125,558,601.0480346679688],"spans":[{"bbox":[303.30694580078125,589.0430908203125,558.4290771484375,601.0480346679688],"content":"netic field lines change their direction from being nearly parallel","score":1,"type":"text"}]},{"bbox":[302,600.0020751953125,558,612.0070190429688],"spans":[{"bbox":[303.30694580078125,600.0020751953125,325.4039611816406,612.0070190429688],"content":"to the","score":1,"type":"text"},{"bbox":[326,602,333,610],"content":"x\\cdot","score":0.72,"type":"inline_equation"},{"bbox":[332.52294921875,600.0020751953125,558.4248657226562,612.0070190429688],"content":"-axis at early times to being mostly perpendicular to it af-","score":1,"type":"text"}]},{"bbox":[302,610.9600830078125,558,622.9650268554688],"spans":[{"bbox":[303.30694580078125,610.9600830078125,558.4290161132812,622.9650268554688],"content":"ter 5 Myr in the neighborhood of the dense layer. In this section,","score":1,"type":"text"}]},{"bbox":[302,621.9191284179688,427.25164794921875,633.924072265625],"spans":[{"bbox":[303.30694580078125,621.9191284179688,427.25164794921875,633.924072265625],"content":"we investigate how this occurs.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[303,653,505,664],"lines":[{"bbox":[303.30694580078125,652.6038818359375,504.53167724609375,664.3209228515625],"spans":[{"bbox":[303.30694580078125,652.6038818359375,504.53167724609375,664.3209228515625],"content":"4.1. Magnetic field amplification by MHD shocks","score":1,"type":"text"}]}],"type":"title"},{"bbox":[302,672.2571411132812,558,760.9750366210938],"lines":[{"bbox":[302,672.2571411132812,558,684.2620849609375],"spans":[{"bbox":[303.30694580078125,672.2571411132812,558.42919921875,684.2620849609375],"content":"As seen in Figure 2, and considering the shock front located at","score":1,"type":"text"}]},{"bbox":[302,683.2161254882812,558,695.2210693359375],"spans":[{"bbox":[303.30694580078125,683.2161254882812,558.42919921875,695.2210693359375],"content":"the right of the condensation layer, we see that the angle between","score":1,"type":"text"}]},{"bbox":[302,694.1751098632812,558,706.1800537109375],"spans":[{"bbox":[303.30694580078125,694.1751098632812,558.4292602539062,706.1800537109375],"content":"the upstream magnetic field and the normal to the shock front","score":1,"type":"text"}]},{"bbox":[302,705,558,717.1390991210938],"spans":[{"bbox":[303.30694580078125,705.1341552734375,334.8585205078125,717.1390991210938],"content":"satisfies","score":1,"type":"text"},{"bbox":[336,705,361,715],"content":"\\theta\\approx0","score":0.89,"type":"inline_equation"},{"bbox":[360.19122314453125,705.1341552734375,558.427001953125,717.1390991210938],"content":" for all the magnetic lines shown. 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The downstream","score":1,"type":"text"}]},{"bbox":[35,497.36651611328125,291,509.3714599609375],"spans":[{"bbox":[36.850006103515625,497.36651611328125,291.9722900390625,509.3714599609375],"content":"flow, just after the shock front, becomes transalfvénic as we can","score":1,"type":"text"}]},{"bbox":[35,508.32550048828125,291,520.3304443359375],"spans":[{"bbox":[36.850006103515625,508.32550048828125,198.93157958984375,520.3304443359375],"content":"see from Figure 2. Therefore the relation","score":1,"type":"text"},{"bbox":[200,509,263,520],"content":"u_{f}>|u_{n}|>u_{A,n}","score":0.94,"type":"inline_equation"},{"bbox":[262.69195556640625,508.32550048828125,291.9720153808594,520.3304443359375],"content":", which","score":1,"type":"text"}]},{"bbox":[35,519.2844848632812,245.88519287109375,531.2894287109375],"spans":[{"bbox":[36.84996032714844,519.2844848632812,245.88519287109375,531.2894287109375],"content":"characterizes a subfast flow, is satisfied downstream.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[35,531.407470703125,291,587.2483520507812],"lines":[{"bbox":[51,531.407470703125,291,543.4124145507812],"spans":[{"bbox":[51.79396057128906,531.407470703125,291.9722900390625,543.4124145507812],"content":"Such MHD shock, going from a superfast to a subfast flow,","score":1,"type":"text"}]},{"bbox":[35,542.366455078125,291,554.3713989257812],"spans":[{"bbox":[36.84996032714844,542.366455078125,291.9721984863281,554.3713989257812],"content":"is called a fast MHD shock (Delmont & Keppens 2011), whose","score":1,"type":"text"}]},{"bbox":[35,553.325439453125,291,565.3303833007812],"spans":[{"bbox":[36.84996032714844,553.325439453125,291.97222900390625,565.3303833007812],"content":"main feature is that it refracts the magnetic field away from the","score":1,"type":"text"}]},{"bbox":[35,564.284423828125,291,576.2893676757812],"spans":[{"bbox":[36.84996032714844,564.284423828125,291.9721984863281,576.2893676757812],"content":"shock normal due to the amplification of the magnetic field com-","score":1,"type":"text"}]},{"bbox":[35,575.243408203125,291,587.2483520507812],"spans":[{"bbox":[36.84996032714844,575.243408203125,291.9721984863281,587.2483520507812],"content":"ponent parallel to the shock front. This amplification is given by","score":1,"type":"text"}]}],"type":"text"},{"bbox":[34,606,152,640],"lines":[{"bbox":[34,606,152,640],"spans":[{"bbox":[34,606,152,640],"content":"B_{\\parallel,2}=\\frac{r_{\\rho}B_{\\parallel,1}(M_{A,1}^{2}-\\cos^{2}\\theta)}{M_{A,1}^{2}-r_{\\rho}\\cos^{2}\\theta},","score":0.93,"type":"interline_equation"}]}],"type":"interline_equation"},{"bbox":[35,650.340576171875,291,760.9755249023438],"lines":[{"bbox":[35,650.340576171875,291,663.8395385742188],"spans":[{"bbox":[36.84999084472656,650.340576171875,61.188621520996094,662.3455200195312],"content":"where","score":1,"type":"text"},{"bbox":[62,651,101,662],"content":"B_{\\parallel,1}=B_{1}","score":0.7,"type":"inline_equation"},{"bbox":[100.79489135742188,650.340576171875,114.5803451538086,663.8395385742188],"content":" sin","score":1,"type":"text"},{"bbox":[115,651,121,660],"content":"\\theta","score":0.26,"type":"inline_equation"},{"bbox":[120.61357879638672,650.340576171875,137.7509765625,662.3455200195312],"content":" and","score":1,"type":"text"},{"bbox":[139,651,155,662],"content":"B_{\\parallel,2}","score":0.9,"type":"inline_equation"},{"bbox":[154.71788024902344,650.340576171875,291.96343994140625,663.8395385742188],"content":" are the upstream and downstream","score":1,"type":"text"}]},{"bbox":[35,661.299560546875,291,673.3045043945312],"spans":[{"bbox":[36.84998321533203,661.299560546875,247.74826049804688,673.3045043945312],"content":"magnetic field components parallel to the shock front,","score":1,"type":"text"},{"bbox":[248,662,291,673],"content":"r_{\\rho}=\\rho_{2}/\\rho_{1}","score":0.91,"type":"inline_equation"}]},{"bbox":[35,672.258544921875,291,684.2634887695312],"spans":[{"bbox":[36.850006103515625,672.258544921875,157.5967254638672,684.2634887695312],"content":"is the ratio of the downstream","score":1,"type":"text"},{"bbox":[159,673,176,684],"content":"(\\rho_{2})","score":0.87,"type":"inline_equation"},{"bbox":[176.2245635986328,672.258544921875,235.98023986816406,684.2634887695312],"content":" and upstream ","score":1,"type":"text"},{"bbox":[235,673,251,684],"content":"(\\rho_{1})","score":0.85,"type":"inline_equation"},{"bbox":[251.6605682373047,672.258544921875,291.96923828125,684.2634887695312],"content":" densities,","score":1,"type":"text"}]},{"bbox":[35,683,291,696.7164916992188],"spans":[{"bbox":[35,683,55,695],"content":"M_{A,1}","score":0.91,"type":"inline_equation"},{"bbox":[55.312923431396484,683.216552734375,275.6275329589844,696.7164916992188],"content":" is the Alfvénic Mach number of the upstream gas, and","score":1,"type":"text"},{"bbox":[275.6275329589844,684.643798828125,278.2190246582031,694.6064453125],"content":" ","score":1,"type":"text"},{"bbox":[277,684,283,693],"content":"\\theta","score":0.73,"type":"inline_equation"},{"bbox":[282.5926208496094,683.216552734375,291.96807861328125,695.2214965820312],"content":" is","score":1,"type":"text"}]},{"bbox":[35,694.1755981445312,291,706.1805419921875],"spans":[{"bbox":[36.85002136230469,694.1755981445312,291.9722595214844,706.1805419921875],"content":"the angle between the vector normal to the front-shock and the","score":1,"type":"text"}]},{"bbox":[35,705,291,717.1395263671875],"spans":[{"bbox":[36.85002136230469,705.1345825195312,131.99282836914062,717.1395263671875],"content":"upstream magnetic field","score":1,"type":"text"},{"bbox":[133,705,147,716],"content":"B_{1}","score":0.88,"type":"inline_equation"},{"bbox":[146.79803466796875,705.1345825195312,291.9730224609375,717.1395263671875],"content":". Since this amplification depends on","score":1,"type":"text"}]},{"bbox":[35,716.0935668945312,291,728.0985107421875],"spans":[{"bbox":[36.85003662109375,716.0935668945312,73.0840072631836,728.0985107421875],"content":"the angle","score":1,"type":"text"},{"bbox":[74,717,80,726],"content":"\\theta","score":0.69,"type":"inline_equation"},{"bbox":[80.0860366821289,716.0935668945312,275.1337585449219,728.0985107421875],"content":", the fluctuating curvature of the shock front at di","score":1,"type":"text"},{"bbox":[275.1320495605469,717.7468872070312,281.109619140625,727.70947265625],"content":"ff","score":1,"type":"text"},{"bbox":[281.1090393066406,716.0935668945312,291.96826171875,728.0985107421875],"content":"er-","score":1,"type":"text"}]},{"bbox":[35,727.0526123046875,291,739.0575561523438],"spans":[{"bbox":[36.85003662109375,727.0526123046875,291.97222900390625,739.0575561523438],"content":"ent positions yields the inhomogeneous downstream magnetic","score":1,"type":"text"}]},{"bbox":[35,738.0115966796875,291,750.0165405273438],"spans":[{"bbox":[36.85003662109375,738.0115966796875,291.9723205566406,750.0165405273438],"content":"field pattern when the shock front travels away from the central","score":1,"type":"text"}]},{"bbox":[35,748.9705810546875,236.03228759765625,760.9755249023438],"spans":[{"bbox":[36.85003662109375,748.9705810546875,236.03228759765625,760.9755249023438],"content":"region, early in the evolution times (see Figure 2).","score":1,"type":"text"}]}],"type":"text"},{"bbox":[302,362.3353271484375,413.41705322265625,374.0523986816406],"lines":[{"bbox":[302,362.3353271484375,413.41705322265625,374.0523986816406],"spans":[{"bbox":[303.3070373535156,362.3353271484375,413.41705322265625,374.0523986816406],"content":"4.2. Line bending analysis","score":1,"type":"text"}]}],"type":"text"},{"bbox":[302,379.50457763671875,558,413.426513671875],"lines":[{"bbox":[302,379.50457763671875,558,391.509521484375],"spans":[{"bbox":[303.3070373535156,379.50457763671875,558.4293212890625,391.509521484375],"content":"To understand how magnetic field lines change their original di-","score":1,"type":"text"}]},{"bbox":[302,390.46258544921875,558,402.467529296875],"spans":[{"bbox":[303.3070373535156,390.46258544921875,558.4292602539062,402.467529296875],"content":"rection in the post-shock region, we consider the induction equa-","score":1,"type":"text"}]},{"bbox":[302,401.42156982421875,379.1323547363281,413.426513671875],"spans":[{"bbox":[303.3070373535156,401.42156982421875,379.1323547363281,413.426513671875],"content":"tion in ideal MHD,","score":1,"type":"text"}]}],"type":"text"},{"bbox":[302,418,465,443],"lines":[{"bbox":[302,418,465,443],"spans":[{"bbox":[302,418,465,443],"content":"\\frac{\\partial\\pmb{B}}{\\partial t}=-\\pmb{B}\\nabla\\cdot\\pmb{u}-(\\pmb{u}\\cdot\\nabla)\\pmb{B}+(\\pmb{B}\\cdot\\nabla)\\pmb{u}.","score":0.93,"type":"interline_equation"}]}],"type":"interline_equation"},{"bbox":[303,458,480,469],"lines":[{"bbox":[303.306884765625,457.82830810546875,479.6495056152344,469.5453796386719],"spans":[{"bbox":[303.306884765625,457.82830810546875,479.6495056152344,469.5453796386719],"content":"4.2.1. Line bending by a compressive flow","score":1,"type":"text"}]}],"type":"title"},{"bbox":[302,474.99755859375,558,563.7153930664062],"lines":[{"bbox":[302,474.99755859375,558,487.00250244140625],"spans":[{"bbox":[303.306884765625,474.99755859375,558.4292602539062,487.00250244140625],"content":"This analysis takes place after the magnetic field component par-","score":1,"type":"text"}]},{"bbox":[302,485.95654296875,558,497.96148681640625],"spans":[{"bbox":[303.306884765625,485.95654296875,558.4290161132812,497.96148681640625],"content":"allel to the shock front is amplified by the fast MHD shock, i.e.,","score":1,"type":"text"}]},{"bbox":[302,496.91552734375,558,508.92047119140625],"spans":[{"bbox":[303.306884765625,496.91552734375,558.4290161132812,508.92047119140625],"content":"in a region containing cooling and thermally unstable gas. Af-","score":1,"type":"text"}]},{"bbox":[302,507.87451171875,558,519.8794555664062],"spans":[{"bbox":[303.306884765625,507.87451171875,558.4292602539062,519.8794555664062],"content":"ter the amplification, magnetic field lines adopt the shape repre-","score":1,"type":"text"}]},{"bbox":[302,518.83349609375,558,530.8384399414062],"spans":[{"bbox":[303.306884765625,518.83349609375,558.42919921875,530.8384399414062],"content":"sented in Figure 5, where the magnetic field component parallel","score":1,"type":"text"}]},{"bbox":[302,529.79248046875,558,541.7974243164062],"spans":[{"bbox":[303.306884765625,529.79248046875,375.05743408203125,541.7974243164062],"content":"to the shock front,","score":1,"type":"text"},{"bbox":[376,530,387,541],"content":"B_{y}","score":0.86,"type":"inline_equation"},{"bbox":[387.2288818359375,529.79248046875,558.4262084960938,541.7974243164062],"content":", has been amplified, and the magnetic field","score":1,"type":"text"}]},{"bbox":[302,540.75146484375,558,554.2504272460938],"spans":[{"bbox":[303.306884765625,540.75146484375,475.9286804199219,552.7564086914062],"content":"component perpendicular to the shock front","score":1,"type":"text"},{"bbox":[477,541,489,552],"content":"B_{x}","score":0.88,"type":"inline_equation"},{"bbox":[487.91326904296875,540.75146484375,558.4244384765625,554.2504272460938],"content":" stays constant, in","score":1,"type":"text"}]},{"bbox":[302,551.71044921875,533.2536010742188,563.7153930664062],"spans":[{"bbox":[303.306884765625,551.71044921875,533.2536010742188,563.7153930664062],"content":"agreement with the jump condition for the magnetic field.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[302,562.66845703125,558,761],"lines":[{"bbox":[318.2508850097656,562.66845703125,558,574.6734008789062],"spans":[{"bbox":[318.2508850097656,562.66845703125,558.42919921875,574.6734008789062],"content":"Furthermore, we assume that the flow speed decreases along","score":1,"type":"text"}]},{"bbox":[302,573.62744140625,558,585.6323852539062],"spans":[{"bbox":[302,576,309,583],"content":"x","score":0.72,"type":"inline_equation"},{"bbox":[308.228271484375,573.62744140625,433.30572509765625,585.6323852539062],"content":" in the post-shock region; i.e.,","score":1,"type":"text"},{"bbox":[433.30572509765625,573.62744140625,437.1528625488281,585.5227661132812],"content":" ","score":1,"type":"text"},{"bbox":[436,574,484,585],"content":"u_{x}~=~u_{x}(x)","score":0.92,"type":"inline_equation"},{"bbox":[483.5093688964844,573.62744140625,501.74090576171875,585.6323852539062],"content":" and","score":1,"type":"text"},{"bbox":[501.74090576171875,575.0546875,505.58184814453125,585.017333984375],"content":" ","score":1,"type":"text"},{"bbox":[504,574,556,585],"content":"\\partial u_{x}/\\partial x\\ <\\ 0","score":0.92,"type":"inline_equation"},{"bbox":[555.9341430664062,573.62744140625,558.4248046875,585.6323852539062],"content":",","score":1,"type":"text"}]},{"bbox":[302,584.58642578125,558,596.5913696289062],"spans":[{"bbox":[303.30682373046875,584.58642578125,558.4291381835938,596.5913696289062],"content":"which represents the compression caused by the cooling of the","score":1,"type":"text"}]},{"bbox":[302,595.54541015625,558,607.5503540039062],"spans":[{"bbox":[303.30682373046875,595.54541015625,558.4291381835938,607.5503540039062],"content":"gas as it travels downstream. Finally, we disregard the down-","score":1,"type":"text"}]},{"bbox":[302,606.5044555664062,558,618.5093994140625],"spans":[{"bbox":[303.30682373046875,606.5044555664062,547.0120239257812,618.5093994140625],"content":"stream component of the velocity parallel to the shock front,","score":1,"type":"text"},{"bbox":[547.0120239257812,606.5044555664062,549.8488159179688,618.3997802734375],"content":" ","score":1,"type":"text"},{"bbox":[549,608,559,618],"content":"u_{y}","score":0.83,"type":"inline_equation"}]},{"bbox":[302,617.4634399414062,558,629.4683837890625],"spans":[{"bbox":[303.30682373046875,617.4634399414062,317.69281005859375,629.4683837890625],"content":"and","score":1,"type":"text"},{"bbox":[319,619,329,629],"content":"u_{z}","score":0.86,"type":"inline_equation"},{"bbox":[329.02081298828125,617.4634399414062,398.8287353515625,629.4683837890625],"content":", to analyze the e","score":1,"type":"text"},{"bbox":[398.82781982421875,619.1167602539062,404.8053894042969,629.079345703125],"content":"ff","score":1,"type":"text"},{"bbox":[404.8048095703125,617.4634399414062,558.4281616210938,629.4683837890625],"content":"ect of the compression alone. To vali-","score":1,"type":"text"}]},{"bbox":[302,628.4224243164062,558,640.4273681640625],"spans":[{"bbox":[303.30682373046875,628.4224243164062,558.4290161132812,640.4273681640625],"content":"date these assumptions, in Figure 6 we plot the relevant physical","score":1,"type":"text"}]},{"bbox":[302,639.3814697265625,558,651.3864135742188],"spans":[{"bbox":[303.30682373046875,639.3814697265625,373.01507568359375,651.3864135742188],"content":"quantities at time","score":1,"type":"text"},{"bbox":[373.01507568359375,639.3814697265625,376.04083251953125,651.2767944335938],"content":" ","score":1,"type":"text"},{"bbox":[375,640,405,650],"content":"t=0.7","score":0.8,"type":"inline_equation"},{"bbox":[405.3020935058594,639.3814697265625,531.3687744140625,651.3864135742188],"content":" Myr along a ray parallel to the","score":1,"type":"text"},{"bbox":[533,641,540,650],"content":"x","score":0.79,"type":"inline_equation"},{"bbox":[539.3181762695312,639.3814697265625,558.4244995117188,651.3864135742188],"content":" axis","score":1,"type":"text"}]},{"bbox":[302,650.3404541015625,558,662.3453979492188],"spans":[{"bbox":[303.3067626953125,650.3404541015625,558.428955078125,662.3453979492188],"content":"passing through a region in which this amplification becomes","score":1,"type":"text"}]},{"bbox":[302,661.2994384765625,558,673.3043823242188],"spans":[{"bbox":[303.3067626953125,661.2994384765625,558.428955078125,673.3043823242188],"content":"large at later evolutionary times. In the top panel, the shock front","score":1,"type":"text"}]},{"bbox":[302,672.2574462890625,558,684.2623901367188],"spans":[{"bbox":[303.3067626953125,672.2574462890625,558.4288940429688,684.2623901367188],"content":"and condensed region are clearly visible in the gas density pro-","score":1,"type":"text"}]},{"bbox":[302,683.2164306640625,558,695.2213745117188],"spans":[{"bbox":[303.3067626953125,683.2164306640625,558.4290771484375,695.2213745117188],"content":"file. The middle panel shows that, in addition to the discontinuity","score":1,"type":"text"}]},{"bbox":[302,694.1754150390625,558,707.6753540039062],"spans":[{"bbox":[303.3067626953125,694.1754150390625,436.84539794921875,706.1803588867188],"content":"at the shocks, the inflow velocity","score":1,"type":"text"},{"bbox":[438,696,450,705],"content":"u_{x}","score":0.85,"type":"inline_equation"},{"bbox":[448.3121032714844,694.1754150390625,558.4247436523438,707.6753540039062],"content":" smoothly decreases down-","score":1,"type":"text"}]},{"bbox":[302,705.1344604492188,558,717.139404296875],"spans":[{"bbox":[303.3067321777344,705.1344604492188,558.428955078125,717.139404296875],"content":"stream from the shock, in sync with the density increase. Also,","score":1,"type":"text"}]},{"bbox":[302,716.0934448242188,558,728.098388671875],"spans":[{"bbox":[302,718,312,728],"content":"u_{y}","score":0.71,"type":"inline_equation"},{"bbox":[311.8827209472656,717.5206909179688,314.3733825683594,727.4833374023438],"content":",","score":1,"type":"text"},{"bbox":[314.3733825683594,716.0934448242188,319.3457336425781,727.98876953125],"content":" ","score":1,"type":"text"},{"bbox":[318,717,348,727],"content":"u_{z}\\,\\approx\\,0","score":0.89,"type":"inline_equation"},{"bbox":[347.4330139160156,716.0934448242188,482.147216796875,728.098388671875],"content":", in agreement with our assumpti","score":1,"type":"text"},{"bbox":[495.9852600097656,716.0934448242188,558.4208984375,728.098388671875],"content":". Finally, in the","score":1,"type":"text"}]},{"bbox":[302,727,558,740.5513916015625],"spans":[{"bbox":[303.3067321777344,727.0524291992188,481.1788635253906,739.057373046875],"content":"bottom panel, we see that the fluctuation of","score":1,"type":"text"},{"bbox":[483,727,495,738],"content":"B_{x}","score":0.89,"type":"inline_equation"},{"bbox":[494.2731018066406,727.0524291992188,558.4292602539062,740.5513916015625],"content":" remains within","score":1,"type":"text"}]},{"bbox":[302,738,558,750.0164184570312],"spans":[{"bbox":[302,738,333,749],"content":"\\lesssim\\,20\\%","score":0.89,"type":"inline_equation"},{"bbox":[332.7591552734375,738.011474609375,558.421875,750.0164184570312],"content":" of its mean value, so it is negligible to the first order.","score":1,"type":"text"}]},{"bbox":[302,748.970458984375,558,761],"spans":[{"bbox":[303.30670166015625,748.970458984375,413.0945129394531,760.9754028320312],"content":"Therefore, the assumptions","score":1,"type":"text"},{"bbox":[413.0945129394531,748.970458984375,416.74169921875,760.8657836914062],"content":" ","score":1,"type":"text"},{"bbox":[415,749,463,761],"content":"B_{y}\\,=\\,B_{y}(x)","score":0.76,"type":"inline_equation"},{"bbox":[462.6882629394531,748.970458984375,465.1789245605469,760.9754028320312],"content":",","score":1,"type":"text"},{"bbox":[465.1789245605469,748.970458984375,468.8227233886719,760.8657836914062],"content":" ","score":1,"type":"text"},{"bbox":[467,749,500,760],"content":"B_{x}\\,=\\,C","score":0.59,"type":"inline_equation"},{"bbox":[500.4847412109375,748.970458984375,530.6116943359375,760.9754028320312],"content":", where","score":1,"type":"text"},{"bbox":[530.6116943359375,748.970458984375,533.6547241210938,760.8657836914062],"content":" ","score":1,"type":"text"},{"bbox":[533,749,541,759],"content":"C","score":0.78,"type":"inline_equation"},{"bbox":[540.2998046875,748.970458984375,558.427734375,760.9754028320312],"content":" is a","score":1,"type":"text"}]}],"type":"text"}]},{"discarded_blocks":[{"bbox":[174,34,420,43],"lines":[{"bbox":[174.968994140625,32.58107376098633,420.3074951171875,43.38558578491211],"spans":[{"bbox":[174.968994140625,32.58107376098633,420.3074951171875,43.38558578491211],"content":"Granda-Muñoz et al.: Magnetic field alignment in interstellar clouds","score":1,"type":"text"}]}],"type":"discarded"},{"bbox":[456,771,558,779],"lines":[{"bbox":[455.1949157714844,769.8160400390625,558.4251098632812,780.6205444335938],"spans":[{"bbox":[455.1949157714844,769.8160400390625,558.4251098632812,780.6205444335938],"content":"Article number, page 5 of 11","score":1,"type":"text"}]}],"type":"discarded"}],"page_idx":4,"page_size":[595.2760009765625,841.8900146484375],"preproc_blocks":[{"bbox":[37,54,558,419],"blocks":[{"bbox":[92,54,503,363],"lines":[{"bbox":[92,54,503,363],"spans":[{"bbox":[92,54,503,363],"image_path":"70d48a8caa72e2a1fb2dba440b843dccd872512362f2236fb151e9e6e515c87a.jpg","score":0.9999694228172302,"type":"image"}]}],"type":"image_body"},{"bbox":[37,370,558,419],"lines":[{"bbox":[36.849998474121094,369.34027099609375,558.4281616210938,381.0055847167969],"spans":[{"bbox":[36.849998474121094,369.34027099609375,60.386802673339844,381.0055847167969],"content":"Fig. 2.","score":1,"type":"text"},{"bbox":[60.386802673339844,369.6630859375,558.4281616210938,380.46759033203125],"content":" The density structure and magnetic field lines of the region R1 are shown after 5 Myr of evolution. The magnetic field lines are colored by","score":1,"type":"text"}]},{"bbox":[36.849998474121094,379.6260986328125,558.42529296875,390.43060302734375],"spans":[{"bbox":[36.849998474121094,379.6260986328125,558.42529296875,390.43060302734375],"content":"the Alfvénic Mach number. Note that at this evolution time, magnetic field lines are almost perpendicular to their original orientation along the","score":1,"type":"text"}]},{"bbox":[36,389.589111328125,558.4230346679688,400.39361572265625],"spans":[{"bbox":[36,391,42,398],"content":"x","score":0.73,"type":"inline_equation"},{"bbox":[41.28008270263672,389.589111328125,558.4230346679688,400.39361572265625],"content":" axis and the change from superalfvénic to transalfvénic of magnetic field lines across the shock. The dark-shaded regions at both sides of the","score":1,"type":"text"}]},{"bbox":[36.849998474121094,399.5511169433594,558.4254760742188,410.3556213378906],"spans":[{"bbox":[36.849998474121094,399.5511169433594,558.4254760742188,410.3556213378906],"content":"center are the shock fronts where magnetic field lines start to bend. 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(7) implies that","score":1,"type":"text"},{"bbox":[210,550,239,561],"content":"d B_{y}/d t","score":0.9,"type":"inline_equation"},{"bbox":[238.99288940429688,549.8035888671875,291.971435546875,561.8085327148438],"content":" has the same","score":1,"type":"text"}]},{"bbox":[36,560.7625732421875,291,574.2615356445312],"spans":[{"bbox":[36.850006103515625,560.7625732421875,64.45636749267578,572.7675170898438],"content":"sign as","score":1,"type":"text"},{"bbox":[64.45636749267578,560.7625732421875,67.50200653076172,572.6578979492188],"content":" ","score":1,"type":"text"},{"bbox":[66,561,77,573],"content":"B_{y}","score":0.87,"type":"inline_equation"},{"bbox":[77.0840072631836,560.7625732421875,256.7893371582031,572.7675170898438],"content":", and therefore the magnetic field component","score":1,"type":"text"},{"bbox":[258,561,269,573],"content":"B_{y}","score":0.88,"type":"inline_equation"},{"bbox":[268.91839599609375,560.7625732421875,291.970458984375,574.2615356445312],"content":" is al-","score":1,"type":"text"}]},{"bbox":[36,571.7215576171875,291,583.7265014648438],"spans":[{"bbox":[36.85002136230469,571.7215576171875,291.97222900390625,583.7265014648438],"content":"ways amplified by the downstream compressive velocity gradi-","score":1,"type":"text"}]},{"bbox":[36,582.6795654296875,291,594.6845092773438],"spans":[{"bbox":[36.85002136230469,582.6795654296875,291.9722595214844,594.6845092773438],"content":"ent. This amplification results in the magnetic field aligning to","score":1,"type":"text"}]},{"bbox":[36,593.6385498046875,205.7858123779297,605.6434936523438],"spans":[{"bbox":[36.85002136230469,593.6385498046875,205.7858123779297,605.6434936523438],"content":"the condensation plane where CACs form.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[36,623,203,633],"lines":[{"bbox":[36.85002136230469,622.0263671875,203.02777099609375,633.743408203125],"spans":[{"bbox":[36.85002136230469,622.0263671875,203.02777099609375,633.743408203125],"content":"4.2.2. Line bending at curved interfaces","score":1,"type":"text"}]}],"type":"title"},{"bbox":[36,639.381591796875,291,760.9755249023438],"lines":[{"bbox":[36,639.381591796875,291,651.3865356445312],"spans":[{"bbox":[36.85002136230469,639.381591796875,291.9722595214844,651.3865356445312],"content":"Another possible mechanism for aligning the magnetic field","score":1,"type":"text"}]},{"bbox":[36,650.340576171875,291,662.3455200195312],"spans":[{"bbox":[36.85002136230469,650.340576171875,291.9722595214844,662.3455200195312],"content":"with the density structures occurs when the collision interface","score":1,"type":"text"}]},{"bbox":[36,661.299560546875,291,673.3045043945312],"spans":[{"bbox":[36.85002136230469,661.299560546875,291.9722900390625,673.3045043945312],"content":"is curved rather than flat, as, for example, in the case of the","score":1,"type":"text"}]},{"bbox":[36,672.258544921875,291,684.2634887695312],"spans":[{"bbox":[36.85002136230469,672.258544921875,291.97222900390625,684.2634887695312],"content":"NTSI (Vishniac 1994). To investigate this, we also ran two-","score":1,"type":"text"}]},{"bbox":[36,683.216552734375,291,695.2214965820312],"spans":[{"bbox":[36.85002136230469,683.216552734375,291.9722900390625,695.2214965820312],"content":"dimensional simulations with the same initial conditions and","score":1,"type":"text"}]},{"bbox":[36,694.175537109375,291,706.1804809570312],"spans":[{"bbox":[36.85002136230469,694.175537109375,291.9722900390625,706.1804809570312],"content":"physics as the three-dimensional simulation described in Sec-","score":1,"type":"text"}]},{"bbox":[36,705.134521484375,291,717.1394653320312],"spans":[{"bbox":[36.85002136230469,705.134521484375,291.9722595214844,717.1394653320312],"content":"tion 2 but with a curved collision interface, obtained by adding","score":1,"type":"text"}]},{"bbox":[36,716.0935668945312,291,728.0985107421875],"spans":[{"bbox":[36.85002136230469,716.0935668945312,291.9722595214844,728.0985107421875],"content":"a sinusoidal displacement perturbation (a “bending mode” per-","score":1,"type":"text"}]},{"bbox":[36,727.0525512695312,291,739.0574951171875],"spans":[{"bbox":[36.85002136230469,727.0525512695312,291.9721984863281,739.0574951171875],"content":"turbation). In the left panel of Figure 7, we show a very early","score":1,"type":"text"}]},{"bbox":[36,738.0115356445312,291,750.0164794921875],"spans":[{"bbox":[36.85002136230469,738.0115356445312,291.9721984863281,750.0164794921875],"content":"stage of this simulation. In this case, the obliqueness of the in-","score":1,"type":"text"}]},{"bbox":[36,748.9705810546875,291,760.9755249023438],"spans":[{"bbox":[36.85002136230469,748.9705810546875,291.9722595214844,760.9755249023438],"content":"terface implies the existence of a component of the incoming","score":1,"type":"text"}]},{"bbox":[303,436.5965576171875,558,448.60150146484375],"spans":[{"bbox":[303.3070068359375,436.5965576171875,558.4292602539062,448.60150146484375],"content":"flow tangential to it, while the perpendicular component is re-","score":1,"type":"text"}]},{"bbox":[303,447.5555419921875,558,459.56048583984375],"spans":[{"bbox":[303.3070068359375,447.5555419921875,558.4293823242188,459.56048583984375],"content":"duced across the shock. This causes the flow to change direction","score":1,"type":"text"}]},{"bbox":[303,458.5145263671875,558,470.51947021484375],"spans":[{"bbox":[303.3070068359375,458.5145263671875,558.4290161132812,470.51947021484375],"content":"at the interface, being now oblique to the original magnetic field","score":1,"type":"text"}]},{"bbox":[303,469.4725341796875,558,481.47747802734375],"spans":[{"bbox":[303.3070068359375,469.4725341796875,558.4290771484375,481.47747802734375],"content":"direction. Being transalfvénic, this oblique post-shock flow can","score":1,"type":"text"}]},{"bbox":[303,480.4315185546875,558,492.43646240234375],"spans":[{"bbox":[303.3070068359375,480.4315185546875,558.4293212890625,492.43646240234375],"content":"begin bending the field lines. The situation is symmetric on both","score":1,"type":"text"}]},{"bbox":[303,491.3905029296875,558,503.39544677734375],"spans":[{"bbox":[303.3070068359375,491.3905029296875,558.4291381835938,503.39544677734375],"content":"sides of the layer, thus generating a shearing velocity field with","score":1,"type":"text"}]},{"bbox":[303,502.3494873046875,558,514.3544311523438],"spans":[{"bbox":[303.3070068359375,502.3494873046875,498.7630920410156,514.3544311523438],"content":"opposite directions at opposite sides due to the di","score":1,"type":"text"},{"bbox":[498.76702880859375,504.0028076171875,504.7445983886719,513.9653930664062],"content":"ff","score":1,"type":"text"},{"bbox":[504.7450256347656,502.3494873046875,558.423583984375,514.3544311523438],"content":"erent concav-","score":1,"type":"text"}]},{"bbox":[303,513.3084716796875,558,525.3134155273438],"spans":[{"bbox":[303.3070068359375,513.3084716796875,558.42919921875,525.3134155273438],"content":"ity of the collision interface. This generates an “S” shape of the","score":1,"type":"text"}]},{"bbox":[303,524.2674560546875,558,536.2723999023438],"spans":[{"bbox":[303.3070068359375,524.2674560546875,558.4293212890625,536.2723999023438],"content":"magnetic field lines across the shocked layer. A later stage of","score":1,"type":"text"}]},{"bbox":[303,535.2264404296875,558,547.2313842773438],"spans":[{"bbox":[303.3070068359375,535.2264404296875,558.4291381835938,547.2313842773438],"content":"this simulation is shown in the right panel of Figure 7, showing","score":1,"type":"text"}]},{"bbox":[303,546.1854248046875,558,558.1903686523438],"spans":[{"bbox":[303.3070068359375,546.1854248046875,558.4293823242188,558.1903686523438],"content":"that the flow tends to be subalfvénic in the condensed regions.","score":1,"type":"text"}]},{"bbox":[303,557.1444091796875,558,569.1493530273438],"spans":[{"bbox":[303.3070068359375,557.1444091796875,519.4454345703125,569.1493530273438],"content":"For this collision interface, the line-bending analysis di","score":1,"type":"text"},{"bbox":[519.447998046875,558.7977294921875,525.425537109375,568.7603149414062],"content":"ff","score":1,"type":"text"},{"bbox":[525.426025390625,557.1444091796875,558.4222412109375,569.1493530273438],"content":"ers from","score":1,"type":"text"}]},{"bbox":[303,568.1033935546875,558,580.1083374023438],"spans":[{"bbox":[303.3070068359375,568.1033935546875,558.4293823242188,580.1083374023438],"content":"that described in Section 4.2. In this case, we will have a ve-","score":1,"type":"text"}]},{"bbox":[303,579.0614013671875,558,591.0663452148438],"spans":[{"bbox":[303.3070068359375,579.0614013671875,558.4291381835938,591.0663452148438],"content":"locity field like the one represented in Figure 8, where the left","score":1,"type":"text"}]},{"bbox":[303,590.0203857421875,558,602.0253295898438],"spans":[{"bbox":[303.3070068359375,590.0203857421875,558.42919921875,602.0253295898438],"content":"panel represents an unperturbed downstream magnetic field line","score":1,"type":"text"}]},{"bbox":[303,600.9793701171875,558,612.9843139648438],"spans":[{"bbox":[303.3070068359375,600.9793701171875,558.4290161132812,612.9843139648438],"content":"and the right panel represents a perturbed one. In the left panel,","score":1,"type":"text"}]},{"bbox":[303,611.9384155273438,558,623.943359375],"spans":[{"bbox":[303.3070068359375,611.9384155273438,558.4293212890625,623.943359375],"content":"we consider a local system of coordinates centered at the point","score":1,"type":"text"}]},{"bbox":[303,622.8973999023438,558,636.3963623046875],"spans":[{"bbox":[303.3070068359375,622.8973999023438,342.1412048339844,634.90234375],"content":"where the","score":1,"type":"text"},{"bbox":[343,624,353,635],"content":"u_{y}","score":0.86,"type":"inline_equation"},{"bbox":[352.54736328125,622.8973999023438,558.4288330078125,636.3963623046875],"content":" is maximum. The magnetic field line is represented","score":1,"type":"text"}]},{"bbox":[303,633.8563842773438,558,645.861328125],"spans":[{"bbox":[303.3070068359375,633.8563842773438,353.4188537597656,645.861328125],"content":"in green, the","score":1,"type":"text"},{"bbox":[355,636,362,644],"content":"x","score":0.73,"type":"inline_equation"},{"bbox":[361.1570129394531,633.8563842773438,503.79144287109375,645.861328125],"content":"-axis is parallel to the field line, the","score":1,"type":"text"},{"bbox":[505,636,512,645],"content":"y","score":0.73,"type":"inline_equation"},{"bbox":[511.00201416015625,633.8563842773438,558.4240112304688,645.861328125],"content":"-axis is per-","score":1,"type":"text"}]},{"bbox":[303,644.8154296875,558,656.8203735351562],"spans":[{"bbox":[303.3070068359375,644.8154296875,558.4292602539062,656.8203735351562],"content":"pendicular to it, and the velocity field is represented by black","score":1,"type":"text"}]},{"bbox":[303,655.7744140625,558,668],"spans":[{"bbox":[303.3070068359375,655.7744140625,394.39501953125,667.7793579101562],"content":"arrows. 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However, a discus-","score":1,"type":"text"}]},{"bbox":[303,426.333251953125,558,438.33819580078125],"spans":[{"bbox":[303.30706787109375,426.333251953125,558.42919921875,438.33819580078125],"content":"sion similar to that in Section 4.2.1 leads us to speculate that the","score":1,"type":"text"}]},{"bbox":[303,437,558,449.29718017578125],"spans":[{"bbox":[302,437,329,448],"content":"\\phi=0^{\\circ}","score":0.91,"type":"inline_equation"},{"bbox":[331.6390686035156,437.292236328125,558.4277954101562,449.29718017578125],"content":"configuration may arise in the presence of a stretching ve-","score":1,"type":"text"}]},{"bbox":[303,448.251220703125,558,460.25616455078125],"spans":[{"bbox":[303.30706787109375,448.251220703125,558.4292602539062,460.25616455078125],"content":"locity field, as it would be the case of the tidal flow into the grav-","score":1,"type":"text"}]},{"bbox":[303,459.210205078125,558,471.21514892578125],"spans":[{"bbox":[303.30706787109375,459.210205078125,558.42919921875,471.21514892578125],"content":"itational well of a strongly self-gravitating cloud. In this case,","score":1,"type":"text"}]},{"bbox":[303,470.169189453125,558,483.6681213378906],"spans":[{"bbox":[302,472,309,480],"content":"x","score":0.67,"type":"inline_equation"},{"bbox":[308.22845458984375,470.169189453125,467.49090576171875,482.17413330078125],"content":" would be the direction of the flow and","score":1,"type":"text"},{"bbox":[469,471,481,482],"content":"B_{y}","score":0.87,"type":"inline_equation"},{"bbox":[480.0664367675781,470.169189453125,558.4236450195312,483.6681213378906],"content":" is a magnetic field","score":1,"type":"text"}]},{"bbox":[303,481.127197265625,558,493.13214111328125],"spans":[{"bbox":[303.30706787109375,481.127197265625,558.4292602539062,493.13214111328125],"content":"perturbation perpendicular to that direction. Therefore, equation","score":1,"type":"text"}]},{"bbox":[303,492,558,504.09112548828125],"spans":[{"bbox":[303.30706787109375,492.086181640625,494.9374694824219,504.09112548828125],"content":"(7) for a positive velocity gradient implies that","score":1,"type":"text"},{"bbox":[494.9374694824219,492.086181640625,498.3570556640625,503.9815368652344],"content":" ","score":1,"type":"text"},{"bbox":[497,492,527,504],"content":"d B_{y}/d t","score":0.91,"type":"inline_equation"},{"bbox":[525.9519653320312,492.086181640625,558.4227294921875,504.09112548828125],"content":" has the","score":1,"type":"text"}]},{"bbox":[303,503,558,515.0501098632812],"spans":[{"bbox":[303.30706787109375,503.045166015625,367.4561767578125,515.0501098632812],"content":"opposite sign to","score":1,"type":"text"},{"bbox":[369,503,380,515],"content":"B_{y}","score":0.88,"type":"inline_equation"},{"bbox":[380.4080505371094,503.045166015625,558.4298095703125,515.0501098632812],"content":", straightening the field lines. Thus, we sug-","score":1,"type":"text"}]},{"bbox":[303,514.004150390625,558,526.0090942382812],"spans":[{"bbox":[303.30706787109375,514.004150390625,558.4290771484375,526.0090942382812],"content":"gest that the induction equation in the presence of a compressive","score":1,"type":"text"}]},{"bbox":[303,524.963134765625,558,536.9680786132812],"spans":[{"bbox":[303.30706787109375,524.963134765625,461.3536071777344,536.9680786132812],"content":"or stretching velocity field leads to the","score":1,"type":"text"},{"bbox":[461.3536071777344,526.390380859375,464.7560729980469,536.35302734375],"content":" ","score":1,"type":"text"},{"bbox":[464,525,509,536],"content":"\\phi\\,=\\,0,90^{\\circ}","score":0.91,"type":"inline_equation"},{"bbox":[511.9290771484375,524.963134765625,558.4246215820312,536.9680786132812],"content":"equilibrium","score":1,"type":"text"}]},{"bbox":[303,535.922119140625,558,547.9270629882812],"spans":[{"bbox":[303.30706787109375,535.922119140625,558.42919921875,547.9270629882812],"content":"configurations found by Soler & Hennebelle (2017), justifying","score":1,"type":"text"}]},{"bbox":[303,546.881103515625,558,558.8860473632812],"spans":[{"bbox":[303.30706787109375,546.881103515625,558.42919921875,558.8860473632812],"content":"their speculation that they may be attractors. 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However, our simulations include strong","score":1,"type":"text"}]},{"bbox":[303,727.0520629882812,558,739.0570068359375],"spans":[{"bbox":[303.3070068359375,727.0520629882812,558.4290161132812,739.0570068359375],"content":"cooling leading to thermal instability, which produces a much","score":1,"type":"text"}]},{"bbox":[303,738.0111083984375,558,750.0160522460938],"spans":[{"bbox":[303.3070068359375,738.0111083984375,558.4292602539062,750.0160522460938],"content":"stronger compression of the condensed layer and a much thin-","score":1,"type":"text"}]},{"bbox":[303,748.9700927734375,558,760.9750366210938],"spans":[{"bbox":[303.3070068359375,748.9700927734375,558.4292602539062,760.9750366210938],"content":"ner slab dimension, even for moderate Mach numbers (Vázquez-","score":1,"type":"text"}]}],"type":"text"}]},{"discarded_blocks":[{"bbox":[173,34,421,43],"lines":[{"bbox":[174.968994140625,32.58107376098633,420.3074951171875,43.38558578491211],"spans":[{"bbox":[174.968994140625,32.58107376098633,420.3074951171875,43.38558578491211],"content":"Granda-Muñoz et al.: Magnetic field alignment in interstellar clouds","score":1,"type":"text"}]}],"type":"discarded"},{"bbox":[454,770,559,780],"lines":[{"bbox":[455.19500732421875,769.81591796875,558.4251708984375,780.6204223632812],"spans":[{"bbox":[455.19500732421875,769.81591796875,558.4251708984375,780.6204223632812],"content":"Article number, page 7 of 11","score":1,"type":"text"}]}],"type":"discarded"}],"page_idx":6,"page_size":[595.2760009765625,841.8900146484375],"preproc_blocks":[{"bbox":[34,53,560,421],"blocks":[{"bbox":[90,53,504,364],"lines":[{"bbox":[90,53,504,364],"spans":[{"bbox":[90,53,504,364],"image_path":"aca9ca0eba0cfc506c1ed152a99dde59fcdfdff8ca6469b58b582da21fa829cf.jpg","score":0.9999658465385437,"type":"image"}]}],"type":"image_body"},{"bbox":[34,369,560,421],"lines":[{"bbox":[36.849998474121094,369.34027099609375,558.4263305664062,381.0055847167969],"spans":[{"bbox":[36.849998474121094,369.34027099609375,61.19377517700195,381.0055847167969],"content":"Fig. 4.","score":1,"type":"text"},{"bbox":[61.19377517700195,369.6630859375,558.4263305664062,380.46759033203125],"content":" Regions used to compute the HRO diagram and the shape parameter shown in Figure 3. 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It can be seen that, for the four density","score":1,"type":"text"}]},{"bbox":[36.850006103515625,399.5511169433594,558.4254150390625,410.3556213378906],"spans":[{"bbox":[36.850006103515625,399.5511169433594,558.4254150390625,410.3556213378906],"content":"intervals shown here, the magnetic field is noticeably parallel to the density structures. However, the magnetic field shows a deviation from this","score":1,"type":"text"}]},{"bbox":[36.850006103515625,409.5141296386719,528.2625122070312,420.3186340332031],"spans":[{"bbox":[36.850006103515625,409.5141296386719,528.2625122070312,420.3186340332031],"content":"trend for the highest density interval in the bottom right panel. 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So, it is not di","score":1,"type":"text"},{"bbox":[184.9320068359375,614.056884765625,193.17108154296875,624.0194702148438],"content":"ffi","score":1,"type":"text"},{"bbox":[193.17100524902344,612.403564453125,291.9700927734375,624.4085083007812],"content":"cult to fulfill the require-","score":1,"type":"text"}]},{"bbox":[36,623.3626098632812,291,635.3675537109375],"spans":[{"bbox":[36.850006103515625,623.3626098632812,218.0796661376953,635.3675537109375],"content":"ment for the development of the NTSI at the","score":1,"type":"text"},{"bbox":[218.0796661376953,623.3626098632812,263.1861267089844,635.2579345703125],"content":" condensed","score":1,"type":"text"},{"bbox":[263.1860046386719,623.3626098632812,291.96795654296875,635.3675537109375],"content":", rather","score":1,"type":"text"}]},{"bbox":[36,634.3215942382812,291,646.3265380859375],"spans":[{"bbox":[36.850006103515625,634.3215942382812,291.97222900390625,646.3265380859375],"content":"than the shocked, layer (Hueckstaedt 2003), as demonstrated by","score":1,"type":"text"}]},{"bbox":[36,645.2805786132812,291,657.2855224609375],"spans":[{"bbox":[36.850006103515625,645.2805786132812,291.9722595214844,657.2855224609375],"content":"the growth of the bending mode perturbation (the increase in","score":1,"type":"text"}]},{"bbox":[36,656.2396240234375,291,668.2445678710938],"spans":[{"bbox":[36.850006103515625,656.2396240234375,291.9722595214844,668.2445678710938],"content":"the curvature) for the dense layer in our 2D simulation. This","score":1,"type":"text"}]},{"bbox":[36,667.1986083984375,291,679.2035522460938],"spans":[{"bbox":[36.850006103515625,667.1986083984375,291.97222900390625,679.2035522460938],"content":"means that NTSI can be triggered by not-so-strong shocks in","score":1,"type":"text"}]},{"bbox":[36,678.1575927734375,138.677734375,690.1625366210938],"spans":[{"bbox":[36.850006103515625,678.1575927734375,138.677734375,690.1625366210938],"content":"the strongly cooling case.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[36,707,273,730],"lines":[{"bbox":[36.850006103515625,708.120361328125,272.42156982421875,719.83740234375],"spans":[{"bbox":[36.850006103515625,708.120361328125,272.42156982421875,719.83740234375],"content":"5.4. The effect of the magnetic field on the NTSI and the","score":1,"type":"text"}]},{"bbox":[55.95500564575195,719.0794067382812,105.30291748046875,730.7964477539062],"spans":[{"bbox":[55.95500564575195,719.0794067382812,105.30291748046875,730.7964477539062],"content":"shear strain","score":1,"type":"text"}]}],"type":"title"},{"bbox":[36,738.0115966796875,291,760.9755249023438],"lines":[{"bbox":[36,738.0115966796875,291,750.0165405273438],"spans":[{"bbox":[36.850006103515625,738.0115966796875,291.9722595214844,750.0165405273438],"content":"The NTSI is one of the possible mechanisms yielding the shear","score":1,"type":"text"}]},{"bbox":[36,748.9705810546875,291,760.9755249023438],"spans":[{"bbox":[36.850006103515625,748.9705810546875,291.9721984863281,760.9755249023438],"content":"strain proposed by Hennebelle (2013) to be responsible for the","score":1,"type":"text"}]},{"bbox":[303,438.42962646484375,558,450.4345703125],"spans":[{"bbox":[303.3070068359375,438.42962646484375,558.42919921875,450.4345703125],"content":"elongation of filamentary CACs and the alignment of these struc-","score":1,"type":"text"}]},{"bbox":[303,449.38861083984375,558,461.3935546875],"spans":[{"bbox":[303.3070068359375,449.38861083984375,558.42919921875,461.3935546875],"content":"tures with the local magnetic field, since it produces the momen-","score":1,"type":"text"}]},{"bbox":[303,460.34759521484375,558,472.3525390625],"spans":[{"bbox":[303.3070068359375,460.34759521484375,558.4291381835938,472.3525390625],"content":"tum transport from the original inflow direction to that parallel","score":1,"type":"text"}]},{"bbox":[303,471.30657958984375,558,483.3115234375],"spans":[{"bbox":[303.3070068359375,471.30657958984375,558.4290161132812,483.3115234375],"content":"to the dense layer in the regions around the nodes, as can be","score":1,"type":"text"}]},{"bbox":[303,482.26556396484375,558,494.2705078125],"spans":[{"bbox":[303.3070068359375,482.26556396484375,558.4292602539062,494.2705078125],"content":"seen in Figure 7. However, Heitsch et al. (2007) found that when","score":1,"type":"text"}]},{"bbox":[303,493.22454833984375,558,505.2294921875],"spans":[{"bbox":[303.3070068359375,493.22454833984375,558.4292602539062,505.2294921875],"content":"the magnetic field is aligned with the inflow, it tends to weaken","score":1,"type":"text"}]},{"bbox":[303,504.18353271484375,558,516.1884765625],"spans":[{"bbox":[303.3070068359375,504.18353271484375,558.4293212890625,516.1884765625],"content":"or even suppress the NTSI due to the magnetic tension coun-","score":1,"type":"text"}]},{"bbox":[303,515.1425170898438,558,527.1474609375],"spans":[{"bbox":[303.3070068359375,515.1425170898438,558.42919921875,527.1474609375],"content":"teracting the transverse momentum transport. Nevertheless, the","score":1,"type":"text"}]},{"bbox":[303,526.1015014648438,558,538.1064453125],"spans":[{"bbox":[303.3070068359375,526.1015014648438,325.44390869140625,538.1064453125],"content":"NTSI","score":1,"type":"text"},{"bbox":[325.44390869140625,526.1015014648438,342.78399658203125,537.996826171875],"content":" can","score":1,"type":"text"},{"bbox":[342.78399658203125,526.1015014648438,558.4205322265625,538.1064453125],"content":" contribute to the change of direction of the magnetic","score":1,"type":"text"}]},{"bbox":[303,537.0604858398438,558,549.0654296875],"spans":[{"bbox":[303.3070068359375,537.0604858398438,558.4291381835938,549.0654296875],"content":"field if the flow surrounding the dense layer, remains at least","score":1,"type":"text"}]},{"bbox":[303,548.0184936523438,558,560.0234375],"spans":[{"bbox":[303.3070068359375,548.0184936523438,426.56427001953125,560.0234375],"content":"transalfvénic, so that it has su","score":1,"type":"text"},{"bbox":[426.56298828125,549.6718139648438,434.80206298828125,559.6343994140625],"content":"ffi","score":1,"type":"text"},{"bbox":[434.802001953125,548.0184936523438,558.4279174804688,560.0234375],"content":"cient energy to bend the field.","score":1,"type":"text"}]},{"bbox":[303,558.9774780273438,558,570.982421875],"spans":[{"bbox":[303.3070068359375,558.9774780273438,558.4292602539062,570.982421875],"content":"This condition is indeed satisfied by the flow between the shock","score":1,"type":"text"}]},{"bbox":[303,569.9364624023438,558,581.94140625],"spans":[{"bbox":[303.3070068359375,569.9364624023438,558.4290771484375,581.94140625],"content":"and the condensation front, as can be seen for the 2D simulation","score":1,"type":"text"}]},{"bbox":[303,580.8954467773438,558,592.900390625],"spans":[{"bbox":[303.3070068359375,580.8954467773438,558.4290161132812,592.900390625],"content":"in both panels of Figure 7. Note, incidentally, that the flow inside","score":1,"type":"text"}]},{"bbox":[303,591.8544921875,462.6687316894531,603.8594360351562],"spans":[{"bbox":[303.3070068359375,591.8544921875,462.6687316894531,603.8594360351562],"content":"the dense layer is generally subalfvénic.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[303,438.42962646484375,558,603.8594360351562],"lines":[],"lines_deleted":true,"type":"text"},{"bbox":[303,606.5044555664062,558,760.9754028320312],"lines":[{"bbox":[318.2510070800781,606.5044555664062,558,618.5093994140625],"spans":[{"bbox":[318.2510070800781,606.5044555664062,558.4293212890625,618.5093994140625],"content":"Another source of shear strain that does not require the NTSI","score":1,"type":"text"}]},{"bbox":[303,617.4634399414062,558,629.4683837890625],"spans":[{"bbox":[303.3070068359375,617.4634399414062,558.42919921875,629.4683837890625],"content":"is observed in our 3D simulation, which does not include an ini-","score":1,"type":"text"}]},{"bbox":[303,628.4224853515625,558,640.4274291992188],"spans":[{"bbox":[303.3070068359375,628.4224853515625,558.4291381835938,640.4274291992188],"content":"tial bending-mode perturbation to the locus of the collision front.","score":1,"type":"text"}]},{"bbox":[303,639.3814697265625,558,651.3864135742188],"spans":[{"bbox":[303.3070068359375,639.3814697265625,558.4292602539062,651.3864135742188],"content":"This arises later in the evolution, when the magnetic field lines","score":1,"type":"text"}]},{"bbox":[303,650.3404541015625,558,662.3453979492188],"spans":[{"bbox":[303.3070068359375,650.3404541015625,558.4293212890625,662.3453979492188],"content":"have already been dragged and bent by the compressive velocity","score":1,"type":"text"}]},{"bbox":[303,661.2994384765625,558,673.3043823242188],"spans":[{"bbox":[303.3070068359375,661.2994384765625,558.42919921875,673.3043823242188],"content":"field. At this time, the transalfvénic condition of the post-shock","score":1,"type":"text"}]},{"bbox":[303,672.2574462890625,558,684.2623901367188],"spans":[{"bbox":[303.3070068359375,672.2574462890625,558.4291381835938,684.2623901367188],"content":"flow allows the magnetic field to partially re-orient the gas flow","score":1,"type":"text"}]},{"bbox":[303,683.2164306640625,558,695.2213745117188],"spans":[{"bbox":[303.3070068359375,683.2164306640625,558.4293212890625,695.2213745117188],"content":"along them. Since the field lines have been oriented nearly par-","score":1,"type":"text"}]},{"bbox":[303,694.1754150390625,558,706.1803588867188],"spans":[{"bbox":[303.3070068359375,694.1754150390625,558.42919921875,706.1803588867188],"content":"allel to the dense layer by the compressive post-shock flow, the","score":1,"type":"text"}]},{"bbox":[303,705.1344604492188,558,717.139404296875],"spans":[{"bbox":[303.3070068359375,705.1344604492188,558.4292602539062,717.139404296875],"content":"velocity field is also oriented in a similar way, and in opposite","score":1,"type":"text"}]},{"bbox":[303,716.0934448242188,558,728.098388671875],"spans":[{"bbox":[303.3070068359375,716.0934448242188,558.4293212890625,728.098388671875],"content":"directions on each side of the dense layer, therefore adding a","score":1,"type":"text"}]},{"bbox":[303,727.0524291992188,558,739.057373046875],"spans":[{"bbox":[303.3070068359375,727.0524291992188,558.4293823242188,739.057373046875],"content":"strong shear component to the flow around the layer. We can","score":1,"type":"text"}]},{"bbox":[303,738.011474609375,558,750.0164184570312],"spans":[{"bbox":[303.3070068359375,738.011474609375,558.4292602539062,750.0164184570312],"content":"see one example of this situation in Figure 9, where the velocity","score":1,"type":"text"}]},{"bbox":[303,748.970458984375,558,760.9754028320312],"spans":[{"bbox":[303.3070068359375,748.970458984375,558.42919921875,760.9754028320312],"content":"fields are represented by dark arrows and the magnetic field lines","score":1,"type":"text"}]}],"type":"text"}]},{"discarded_blocks":[{"bbox":[37,771,139,779],"lines":[{"bbox":[36.850006103515625,769.8160400390625,140.08016967773438,780.6205444335938],"spans":[{"bbox":[36.850006103515625,769.8160400390625,140.08016967773438,780.6205444335938],"content":"Article number, page 8 of 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The two color bars represent the number density and the Alfvénic Mach number.","score":1,"type":"text"}]}],"type":"image_caption"}],"type":"image"},{"bbox":[36,697.2095947265625,291,753.0494995117188],"lines":[{"bbox":[36,697.2095947265625,291,709.2145385742188],"spans":[{"bbox":[36.849998474121094,697.2095947265625,291.9722595214844,709.2145385742188],"content":"are color-coded with the Alfvénic Mach number. In this Figure,","score":1,"type":"text"}]},{"bbox":[36,708.1685791015625,291,720.1735229492188],"spans":[{"bbox":[36.849998474121094,708.1685791015625,291.9721984863281,720.1735229492188],"content":"the troughs and peaks of the CACs do not show corresponding","score":1,"type":"text"}]},{"bbox":[36,719.1275634765625,291,731.1325073242188],"spans":[{"bbox":[36.849998474121094,719.1275634765625,291.97222900390625,731.1325073242188],"content":"converging and diverging velocity fields, as would correspond to","score":1,"type":"text"}]},{"bbox":[36,730.0855712890625,291,742.0905151367188],"spans":[{"bbox":[36.849998474121094,730.0855712890625,291.9722900390625,742.0905151367188],"content":"the NTSI, and so the structure at this point appears not have been","score":1,"type":"text"}]},{"bbox":[36,741.0445556640625,139.15589904785156,753.0494995117188],"spans":[{"bbox":[36.849998474121094,741.0445556640625,139.15589904785156,753.0494995117188],"content":"formed by this instability.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[303,697.3953857421875,553.9365234375,709.1124267578125],"lines":[{"bbox":[303,697.3953857421875,553.9365234375,709.1124267578125],"spans":[{"bbox":[303.3070068359375,697.3953857421875,553.9365234375,709.1124267578125],"content":"5.5. 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Comparison with previous work","score":1,"type":"text"}]}],"type":"title"},{"bbox":[36,326.7995910644531,291,415.5164794921875],"lines":[{"bbox":[36,326.7995910644531,291,338.8045349121094],"spans":[{"bbox":[36.849998474121094,326.7995910644531,291.97222900390625,338.8045349121094],"content":"The superalfvénic nature of the initial inflow in our simulations,","score":1,"type":"text"}]},{"bbox":[36,337.75860595703125,291,349.7635498046875],"spans":[{"bbox":[36.849998474121094,337.75860595703125,291.9722595214844,349.7635498046875],"content":"and its continuation downstream as a transalfvénic flow, allow","score":1,"type":"text"}]},{"bbox":[36,348.71759033203125,291,360.7225341796875],"spans":[{"bbox":[36.849998474121094,348.71759033203125,291.9722900390625,360.7225341796875],"content":"the dragging and amplification of the magnetic field, in agree-","score":1,"type":"text"}]},{"bbox":[36,359.67559814453125,291,371.6805419921875],"spans":[{"bbox":[36.849998474121094,359.67559814453125,291.9721984863281,371.6805419921875],"content":"ment with Skalidis et al. 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How-","score":1,"type":"text"}]},{"bbox":[36,436.633544921875,291,448.63848876953125],"spans":[{"bbox":[36.8499755859375,436.633544921875,291.9722595214844,448.63848876953125],"content":"ever, the main physical processes responsible for the alignment","score":1,"type":"text"}]},{"bbox":[36,447.592529296875,291,459.59747314453125],"spans":[{"bbox":[36.8499755859375,447.592529296875,291.9722595214844,459.59747314453125],"content":"of magnetic field lines and density structures, MHD shocks, and","score":1,"type":"text"}]},{"bbox":[36,458.551513671875,291,470.55645751953125],"spans":[{"bbox":[36.8499755859375,458.551513671875,291.9722595214844,470.55645751953125],"content":"the NTSI, can be also present at the interfaces between interact-","score":1,"type":"text"}]},{"bbox":[36,469.510498046875,291,481.51544189453125],"spans":[{"bbox":[36.8499755859375,469.510498046875,150.64280700683594,481.51544189453125],"content":"ing wind-blown bubbles and","score":1,"type":"text"},{"bbox":[150.64097595214844,471.163818359375,153.3607635498047,481.1264343261719],"content":"/","score":1,"type":"text"},{"bbox":[153.36097717285156,469.510498046875,291.9706115722656,481.51544189453125],"content":"or supernova shells. Therefore, the","score":1,"type":"text"}]},{"bbox":[36,480.468505859375,291,492.47344970703125],"spans":[{"bbox":[36.8499755859375,480.468505859375,291.9721984863281,492.47344970703125],"content":"MHD shocks and the NTSI could also be the principal physi-","score":1,"type":"text"}]},{"bbox":[36,491.427490234375,291,503.43243408203125],"spans":[{"bbox":[36.8499755859375,491.427490234375,291.97222900390625,503.43243408203125],"content":"cal mechanisms behind the magnetic field alignment with fibers","score":1,"type":"text"}]},{"bbox":[36,502.386474609375,234.97616577148438,514.3914184570312],"spans":[{"bbox":[36.8499755859375,502.386474609375,234.97616577148438,514.3914184570312],"content":"found in this type of object by Clark et al. (2014).","score":1,"type":"text"}]}],"type":"text"},{"bbox":[36,534,182,545],"lines":[{"bbox":[36.8499755859375,532.9898681640625,182.31346130371094,546.006591796875],"spans":[{"bbox":[36.8499755859375,532.9898681640625,182.31346130371094,546.006591796875],"content":"6. Summary and Conclusions","score":1,"type":"text"}]}],"type":"title"},{"bbox":[36,551.219482421875,291,639.9373779296875],"lines":[{"bbox":[36,551.219482421875,291,563.2244262695312],"spans":[{"bbox":[36.8499755859375,551.219482421875,291.97222900390625,563.2244262695312],"content":"In this work, we have studied the physical mechanisms responsi-","score":1,"type":"text"}]},{"bbox":[36,562.178466796875,291,574.1834106445312],"spans":[{"bbox":[36.8499755859375,562.178466796875,291.97222900390625,574.1834106445312],"content":"ble for the observed alignment of magnetic field and cold atomic","score":1,"type":"text"}]},{"bbox":[36,573.137451171875,291,585.1423950195312],"spans":[{"bbox":[36.8499755859375,573.137451171875,291.9721984863281,585.1423950195312],"content":"gravitationally unbound density structures formed by the colli-","score":1,"type":"text"}]},{"bbox":[36,584.096435546875,291,596.1013793945312],"spans":[{"bbox":[36.8499755859375,584.096435546875,291.9722595214844,596.1013793945312],"content":"sion of converging warm atomic gas. We have tracked the evo-","score":1,"type":"text"}]},{"bbox":[36,595.055419921875,291,607.0603637695312],"spans":[{"bbox":[36.8499755859375,595.055419921875,291.9721984863281,607.0603637695312],"content":"lution of magnetic field lines in a three-dimensional simulation","score":1,"type":"text"}]},{"bbox":[36,606.0144653320312,291,618.0194091796875],"spans":[{"bbox":[36.8499755859375,606.0144653320312,291.9721374511719,618.0194091796875],"content":"having typical conditions of the warm ISM and found that they","score":1,"type":"text"}]},{"bbox":[36,616.9734497070312,291,628.9783935546875],"spans":[{"bbox":[36.8499755859375,616.9734497070312,291.97222900390625,628.9783935546875],"content":"become perpendicular to their original orientation and end up","score":1,"type":"text"}]},{"bbox":[36,627.9324340820312,161.37249755859375,639.9373779296875],"spans":[{"bbox":[36.8499755859375,627.9324340820312,161.37249755859375,639.9373779296875],"content":"aligned with density structures.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[36,639.136474609375,291,694.8667602539062],"lines":[{"bbox":[51,639.136474609375,291,651.1414184570312],"spans":[{"bbox":[51.793975830078125,639.136474609375,291.9723205566406,651.1414184570312],"content":"The process of the alignment of magnetic field lines with","score":1,"type":"text"}]},{"bbox":[36,650.095458984375,291,662.1004028320312],"spans":[{"bbox":[36.8499755859375,650.095458984375,122.99655151367188,662.1004028320312],"content":"the density structures","score":1,"type":"text"},{"bbox":[122.99655151367188,650.095458984375,226.50059509277344,661.9907836914062],"content":" starts at the shock fronts","score":1,"type":"text"},{"bbox":[226.50059509277344,650.095458984375,291.96734619140625,662.1004028320312],"content":" and takes place","score":1,"type":"text"}]},{"bbox":[36,661.053466796875,291,672.9487915039062],"spans":[{"bbox":[36.8499755859375,661.053466796875,291.9721984863281,672.9487915039062],"content":"in the cooling, thermally unstable gas, so that the magnetic field","score":1,"type":"text"}]},{"bbox":[36,672.012451171875,291,683.9077758789062],"spans":[{"bbox":[36.8499755859375,672.012451171875,291.97222900390625,683.9077758789062],"content":"already shows a preferred orientation when the flow forms CACs","score":1,"type":"text"}]},{"bbox":[36,682.971435546875,128.15719604492188,694.8667602539062],"spans":[{"bbox":[36.8499755859375,682.971435546875,128.15719604492188,694.8667602539062],"content":"at the condensed layer.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[36,694.1754150390625,291,760.9754028320312],"lines":[{"bbox":[51,694.1754150390625,291,706.1803588867188],"spans":[{"bbox":[51.793975830078125,694.1754150390625,291.9723205566406,706.1803588867188],"content":"At the position of the shocks, the magnetic field changes its","score":1,"type":"text"}]},{"bbox":[36,705.1343994140625,291,717.1393432617188],"spans":[{"bbox":[36.8499755859375,705.1343994140625,291.97216796875,717.1393432617188],"content":"direction due to the amplification of its component parallel to","score":1,"type":"text"}]},{"bbox":[36,716.0934448242188,291,728.098388671875],"spans":[{"bbox":[36.8499755859375,716.0934448242188,291.97216796875,728.098388671875],"content":"the front, which is produced by the velocity fluctuations in the","score":1,"type":"text"}]},{"bbox":[36,727.0524291992188,291,739.057373046875],"spans":[{"bbox":[36.8499755859375,727.0524291992188,291.97222900390625,739.057373046875],"content":"pre-shock region. This amplification occurs due to a fast MHD","score":1,"type":"text"}]},{"bbox":[36,738.0114135742188,291,750.016357421875],"spans":[{"bbox":[36.8499755859375,738.0114135742188,291.97222900390625,750.016357421875],"content":"shock that occurs when the upstream and downstream flows are","score":1,"type":"text"}]},{"bbox":[36,748.970458984375,168.5854034423828,760.9754028320312],"spans":[{"bbox":[36.8499755859375,748.970458984375,168.5854034423828,760.9754028320312],"content":"super– and sub-fast, respectively.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[303,56.56640625,558,167.2012176513672],"lines":[{"bbox":[318,56.56640625,558,68.57134246826172],"spans":[{"bbox":[318.2509765625,56.56640625,558.4293212890625,68.57134246826172],"content":"Behind the shock front, the compressive downstream veloc-","score":1,"type":"text"}]},{"bbox":[303,67.525390625,558,79.53032684326172],"spans":[{"bbox":[303.3069763183594,67.525390625,558.4292602539062,79.53032684326172],"content":"ity field further amplifies the magnetic field component parallel","score":1,"type":"text"}]},{"bbox":[303,78.484375,558,90.48931121826172],"spans":[{"bbox":[303.3069763183594,78.484375,558.4290161132812,90.48931121826172],"content":"to the shock front, increasing the curvature of the lines in this","score":1,"type":"text"}]},{"bbox":[303,89.443359375,558,101.44829559326172],"spans":[{"bbox":[303.3069763183594,89.443359375,558.4291381835938,101.44829559326172],"content":"region, and causing them to become increasingly parallel to the","score":1,"type":"text"}]},{"bbox":[303,100.40234375,558,112.40727996826172],"spans":[{"bbox":[303.3069763183594,100.40234375,558.4291381835938,112.40727996826172],"content":"condensed layer produced by the thermal instability. The ampli-","score":1,"type":"text"}]},{"bbox":[303,111.361328125,558,123.36626434326172],"spans":[{"bbox":[303.3069763183594,111.361328125,558.4292602539062,123.36626434326172],"content":"fication of the fluctuation by a compressive velocity gradient can","score":1,"type":"text"}]},{"bbox":[303,122.3203125,558,134.3252410888672],"spans":[{"bbox":[303.3069763183594,122.3203125,558.4290771484375,134.3252410888672],"content":"be understood through an analysis of the induction equation for","score":1,"type":"text"}]},{"bbox":[303,133.279296875,558,145.2842254638672],"spans":[{"bbox":[303.3069763183594,133.279296875,558.4292602539062,145.2842254638672],"content":"planar geometry (eq. [7]), which shows that the change in the","score":1,"type":"text"}]},{"bbox":[303,144.2373046875,558,156.2422332763672],"spans":[{"bbox":[303.3069763183594,144.2373046875,558.4293212890625,156.2422332763672],"content":"fluctuating field component has the same sign as the fluctuation,","score":1,"type":"text"}]},{"bbox":[303,155.1962890625,357.55328369140625,167.2012176513672],"spans":[{"bbox":[303.3069763183594,155.1962890625,357.55328369140625,167.2012176513672],"content":"amplifying it.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[303,166.1552734375,558,265.83209228515625],"lines":[{"bbox":[318,166.1552734375,558,178.1602020263672],"spans":[{"bbox":[318.2509765625,166.1552734375,558.429443359375,178.1602020263672],"content":"From the same equation, we concluded that a stretching ve-","score":1,"type":"text"}]},{"bbox":[303,177.1142578125,558,189.1191864013672],"spans":[{"bbox":[303.3069763183594,177.1142578125,392.9504089355469,189.1191864013672],"content":"locity gradient causes","score":1,"type":"text"},{"bbox":[392.9504089355469,177.1142578125,431.9690246582031,189.0095977783203],"content":" damping","score":1,"type":"text"},{"bbox":[431.9690246582031,177.1142578125,558.4298706054688,189.1191864013672],"content":" of the fluctuating component,","score":1,"type":"text"}]},{"bbox":[303,188.0732421875,558,200.0781707763672],"spans":[{"bbox":[303.3070068359375,188.0732421875,558.4291381835938,200.0781707763672],"content":"leading to a straightening of the field lines, thus orienting them","score":1,"type":"text"}]},{"bbox":[303,199.0322265625,558,211.0371551513672],"spans":[{"bbox":[303.3070068359375,199.0322265625,359.75506591796875,210.9275665283203],"content":"perpendicular","score":1,"type":"text"},{"bbox":[359.75506591796875,199.0322265625,558.4254760742188,211.0371551513672],"content":" to the density structures. We speculate that this is","score":1,"type":"text"}]},{"bbox":[303,209.9912109375,558,221.9961395263672],"spans":[{"bbox":[303.3070068359375,209.9912109375,558.42919921875,221.9961395263672],"content":"the mechanism occurring during the growth of self-gravitating","score":1,"type":"text"}]},{"bbox":[303,220.9501953125,558,232.9551239013672],"spans":[{"bbox":[303.3070068359375,220.9501953125,408.6913757324219,232.9551239013672],"content":"structures, where the flow","score":1,"type":"text"},{"bbox":[408.6913757324219,220.9501953125,457.3052673339844,232.8455352783203],"content":" accelerates","score":1,"type":"text"},{"bbox":[457.3052673339844,220.9501953125,558.4212646484375,232.9551239013672],"content":" inwards, thus producing","score":1,"type":"text"}]},{"bbox":[303,231.9091796875,558,243.9141082763672],"spans":[{"bbox":[303.3070068359375,231.9091796875,558.4291381835938,243.9141082763672],"content":"a tidal stretching velocity pattern, thus being a possible expla-","score":1,"type":"text"}]},{"bbox":[303,242.8681640625,558,254.8730926513672],"spans":[{"bbox":[303.3070068359375,242.8681640625,558.4290771484375,254.8730926513672],"content":"nation for the perpendicular orientation of the field lines around","score":1,"type":"text"}]},{"bbox":[303,253.8271484375,472.45196533203125,265.83209228515625],"spans":[{"bbox":[303.3070068359375,253.8271484375,472.45196533203125,265.83209228515625],"content":"self-gravitating molecular cloud filaments.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[303,264.78515625,558,353.50299072265625],"lines":[{"bbox":[318,264.78515625,558,276.79010009765625],"spans":[{"bbox":[318.2510070800781,264.78515625,462.8480529785156,276.79010009765625],"content":"In conclusion, we have found that a","score":1,"type":"text"},{"bbox":[462.8480529785156,264.78515625,495.1838073730469,276.6805114746094],"content":" settling","score":1,"type":"text"},{"bbox":[495.1838073730469,264.78515625,558.4208984375,276.79010009765625],"content":" (i.e., decelerat-","score":1,"type":"text"}]},{"bbox":[303,275.744140625,558,287.74908447265625],"spans":[{"bbox":[303.3070068359375,275.744140625,558.42919921875,287.74908447265625],"content":"ing) flow, such as that occurring due to the condensation of the","score":1,"type":"text"}]},{"bbox":[303,286.703125,558,298.70806884765625],"spans":[{"bbox":[303.3070068359375,286.703125,558.42919921875,298.70806884765625],"content":"gas by thermal instability orients the lines parallel to the density","score":1,"type":"text"}]},{"bbox":[303,297.662109375,558,309.66705322265625],"spans":[{"bbox":[303.3070068359375,297.662109375,378.3054504394531,309.66705322265625],"content":"structures, while a","score":1,"type":"text"},{"bbox":[378.3054504394531,297.662109375,421.25030517578125,309.5574645996094],"content":" stretching","score":1,"type":"text"},{"bbox":[421.25030517578125,297.662109375,558.4276123046875,309.66705322265625],"content":" (accelerating) one, such as infall","score":1,"type":"text"}]},{"bbox":[303,308.62109375,558,320.62603759765625],"spans":[{"bbox":[303.3070068359375,308.62109375,558.42919921875,320.62603759765625],"content":"into a potential well, orients the field lines perpendicular to the","score":1,"type":"text"}]},{"bbox":[303,319.580078125,558,331.58502197265625],"spans":[{"bbox":[303.3070068359375,319.580078125,558.4292602539062,331.58502197265625],"content":"density structures. This may be the physical mechanism behind","score":1,"type":"text"}]},{"bbox":[303,330.5390625,558,342.54400634765625],"spans":[{"bbox":[303.3070068359375,330.5390625,558.42919921875,342.54400634765625],"content":"the stationarity of these configurations found by Soler & Hen-","score":1,"type":"text"}]},{"bbox":[303,341.498046875,363.62054443359375,353.50299072265625],"spans":[{"bbox":[303.3070068359375,341.498046875,363.62054443359375,353.50299072265625],"content":"nebelle (2017).","score":1,"type":"text"}]}],"type":"text"},{"bbox":[303,352.45703125,558,397.33795166015625],"lines":[{"bbox":[318,352.45703125,558,364.46197509765625],"spans":[{"bbox":[318.2510070800781,352.45703125,558.4293212890625,364.46197509765625],"content":"Finally, we also found that, under typical conditions of the","score":1,"type":"text"}]},{"bbox":[303,363.416015625,558,375.42095947265625],"spans":[{"bbox":[303.3070068359375,363.416015625,558.4293823242188,375.42095947265625],"content":"ISM, the flow upstream from the shock front is superalfvénic","score":1,"type":"text"}]},{"bbox":[303,374.3740234375,558,386.37896728515625],"spans":[{"bbox":[303.3070068359375,374.3740234375,558.4293823242188,386.37896728515625],"content":"and becomes transalfvénic downstream. This allows the velocity","score":1,"type":"text"}]},{"bbox":[303,385.3330078125,487.8741455078125,397.33795166015625],"spans":[{"bbox":[303.3070068359375,385.3330078125,487.8741455078125,397.33795166015625],"content":"field to bend and drag the magnetic field lines.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[303,402.0290832519531,558,464.89312744140625],"lines":[{"bbox":[303,402.0290832519531,558,411.633056640625],"spans":[{"bbox":[303.3070068359375,402.0290832519531,366.1512756347656,411.5453796386719],"content":"Acknowledgements.","score":1,"type":"text"},{"bbox":[366.1512756347656,402.0290832519531,558.4215698242188,411.633056640625],"content":" We are grateful to Susan Clark and Laura Fissel for use-","score":1,"type":"text"}]},{"bbox":[303,410.90509033203125,558,420.5090637207031],"spans":[{"bbox":[303.3070068359375,410.90509033203125,558.4219970703125,420.5090637207031],"content":"ful comments and suggestions. This research was supported by a CONACYT","score":1,"type":"text"}]},{"bbox":[303,419.7821044921875,558,429.3860778808594],"spans":[{"bbox":[303.3070068359375,419.7821044921875,558.4220581054688,429.3860778808594],"content":"scholarship. GCG and EVS acknowledge support from UNAM-PAPIIT grants","score":1,"type":"text"}]},{"bbox":[303,428.65911865234375,558,438.2630920410156],"spans":[{"bbox":[303.3070068359375,428.65911865234375,558.4220581054688,438.2630920410156],"content":"IN103822 and IG100223, respectively. In addition, we acknowledge Interstellar","score":1,"type":"text"}]},{"bbox":[303,437.5351257324219,558,447.13909912109375],"spans":[{"bbox":[303.3070068359375,437.5351257324219,558.4220581054688,447.13909912109375],"content":"Institute’s program “With Two Eyes” and the Paris-Saclay University’s Institut","score":1,"type":"text"}]},{"bbox":[303,446.4121398925781,558,456.01611328125],"spans":[{"bbox":[303.3070068359375,446.4121398925781,558.4220581054688,456.01611328125],"content":"Pascal for hosting discussions that nourished the development of the ideas behind","score":1,"type":"text"}]},{"bbox":[303,455.2891540527344,337,464.89312744140625],"spans":[{"bbox":[303.3070068359375,455.2891540527344,335.10772705078125,464.89312744140625],"content":"this work.","score":1,"type":"text"}]}],"type":"text"},{"bbox":[303,492,359,503],"lines":[{"bbox":[303.3070068359375,491.6244812011719,359.0736083984375,504.64117431640625],"spans":[{"bbox":[303.3070068359375,491.6244812011719,359.0736083984375,504.64117431640625],"content":"References","score":1,"type":"text"}]}],"type":"title"},{"bbox":[303,509.4581298828125,558,760.4152221679688],"lines":[{"bbox":[303,509.4581298828125,451,519.0621337890625],"spans":[{"bbox":[303.3070068359375,509.4581298828125,451.853759765625,519.0621337890625],"content":"Audit, E. & Hennebelle, P. 2005, A&A, 433, 1","score":1,"type":"text"}]},{"bbox":[303,518.3851318359375,467.8258361816406,527.9891357421875],"spans":[{"bbox":[303.3070068359375,518.3851318359375,467.8258361816406,527.9891357421875],"content":"Blondin, J. 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d1ce80af..5efbb904 100644 --- a/projects/web_api/web_api/api/__init__.py +++ b/projects/web_api/web_api/api/__init__.py @@ -4,7 +4,7 @@ from common.web_hook import before_request from common.logger import setup_log root_dir = os.path.dirname(os.path.dirname(os.path.abspath(__file__))) -print("root_dir", root_dir) + def _register_db(flask_app): from common import import_models @@ -30,6 +30,8 @@ def create_app(config): ma.init_app(app=app) from .analysis import analysis_blue app.register_blueprint(analysis_blue) + from .react_app import react_app_blue + app.register_blueprint(react_app_blue) app.before_request(before_request) diff --git a/projects/web_api/web_api/api/analysis/__init__.py b/projects/web_api/web_api/api/analysis/__init__.py index 93b7ea04..309d8e7a 100644 --- a/projects/web_api/web_api/api/analysis/__init__.py +++ b/projects/web_api/web_api/api/analysis/__init__.py @@ -4,6 +4,7 @@ from .upload_view import UploadPdfView from .analysis_view import AnalysisTaskView, AnalysisTaskProgressView from .img_md_view import ImgView, MdView from .task_view import TaskView, HistoricalTasksView, DeleteTaskView +from .markdown_view import MarkdownView analysis_blue = Blueprint('analysis', __name__) @@ -15,4 +16,5 @@ api_v2.add_resource(ImgView, '/analysis/pdf_img') api_v2.add_resource(MdView, '/analysis/pdf_md') api_v2.add_resource(TaskView, '/extract/taskQueue') api_v2.add_resource(HistoricalTasksView, '/extract/list') -api_v2.add_resource(DeleteTaskView, '/extract/task/') \ No newline at end of file +api_v2.add_resource(DeleteTaskView, '/extract/task/') +api_v2.add_resource(MarkdownView, '/extract/markdown') \ No newline at end of file diff --git a/projects/web_api/web_api/api/analysis/analysis_view.py b/projects/web_api/web_api/api/analysis/analysis_view.py index a9747c8b..f2b9d451 100644 --- a/projects/web_api/web_api/api/analysis/analysis_view.py +++ b/projects/web_api/web_api/api/analysis/analysis_view.py @@ -1,5 +1,6 @@ import json import threading +from multiprocessing import Process from pathlib import Path from flask import request, current_app, url_for from flask_restful import Resource @@ -212,10 +213,10 @@ class AnalysisTaskView(Resource): pdf_analysis_folder = current_app.config['PDF_ANALYSIS_FOLDER'] pdf_dir = f"{current_app.static_folder}/{pdf_analysis_folder}/{file_stem}" image_dir = f"{pdf_dir}/images" - t = threading.Thread(target=analysis_pdf_task, - args=(pdf_dir, image_dir, file_path, analysis_task.is_ocr, - analysis_task.analysis_pdf_id)) - t.start() + process = Process(target=analysis_pdf_task, + args=(pdf_dir, image_dir, file_path, analysis_task.is_ocr, + analysis_task.analysis_pdf_id)) + process.start() # 生成文件的URL路径 file_url = url_for('analysis.uploadpdfview', filename=analysis_task.file_name, as_attachment=False) diff --git a/projects/web_api/web_api/api/analysis/markdown_view.py b/projects/web_api/web_api/api/analysis/markdown_view.py new file mode 100644 index 00000000..d82d95b2 --- /dev/null +++ b/projects/web_api/web_api/api/analysis/markdown_view.py @@ -0,0 +1,44 @@ +import json +from pathlib import Path +from flask import request, current_app +from flask_restful import Resource +from common.custom_response import generate_response + + +class MarkdownView(Resource): + + def put(self): + """ + 编辑markdown + """ + params = json.loads(request.data) + file_key = params.get('file_key') + data = params.get('data', {}) + if not data: + return generate_response(code=400, msg="empty data", msgZH="数据为空，无法更新markdown") + + pdf_analysis_folder = current_app.config['PDF_ANALYSIS_FOLDER'] + pdf_dir = f"{current_app.static_folder}/{pdf_analysis_folder}" + markdown_file_dir = "" + for path_obj in Path(pdf_dir).iterdir(): + if path_obj.name.startswith(file_key): + markdown_file_dir = path_obj + break + + if markdown_file_dir and Path(markdown_file_dir).exists(): + for k, v in data.items(): + md_path = f"{markdown_file_dir}/{k}.md" + if Path(md_path).exists(): + with open(md_path, 'w', encoding="utf-8") as f: + f.write(v) + + full_content = "" + for path_obj in Path(markdown_file_dir).iterdir(): + if path_obj.is_file() and path_obj.suffix == ".md" and path_obj.stem != "full": + with open(path_obj, 'r', encoding="utf-8") as f: + full_content += f.read() + "\n" + with open(f"{markdown_file_dir}/full.md", 'w', encoding="utf-8") as f: + f.write(full_content) + else: + return generate_response(code=400, msg="Invalid file_key", msgZH="文件哈希错误") + return generate_response() diff --git a/projects/web_api/web_api/api/extentions.py b/projects/web_api/web_api/api/extentions.py index 643b582b..0d5fcb01 100644 --- a/projects/web_api/web_api/api/extentions.py +++ b/projects/web_api/web_api/api/extentions.py @@ -59,3 +59,4 @@ db = SQLAlchemy() migrate = Migrate() jwt = JWTManager() ma = Marshmallow() +folder = app.config.get("REACT_APP_DIST") diff --git a/projects/web_api/web_api/api/react_app/__init__.py b/projects/web_api/web_api/api/react_app/__init__.py new file mode 100644 index 00000000..b93589a0 --- /dev/null +++ b/projects/web_api/web_api/api/react_app/__init__.py @@ -0,0 +1,11 @@ +from pathlib import Path +from flask import Blueprint +from ..extentions import app, Api +from .react_app_view import ReactAppView +from loguru import logger + +folder = Path(app.config.get("REACT_APP_DIST", "../../web/dist/")).resolve() +logger.info(f"react_app folder: {folder}") +react_app_blue = Blueprint('react_app', __name__, static_folder=folder, static_url_path='', template_folder=folder) +react_app_api = Api(react_app_blue, prefix='') +react_app_api.add_resource(ReactAppView, '/') \ No newline at end of file diff --git a/projects/web_api/web_api/api/react_app/react_app_view.py b/projects/web_api/web_api/api/react_app/react_app_view.py new file mode 100644 index 00000000..7c2ff82a --- /dev/null +++ b/projects/web_api/web_api/api/react_app/react_app_view.py @@ -0,0 +1,11 @@ +from flask import render_template, Response +from flask_restful import Resource + + +class ReactAppView(Resource): + def get(self): + # 创建自定义的响应对象 + rendered_template = render_template('index.html') + response = Response(rendered_template, mimetype='text/html') + + return response diff --git a/projects/web_api/web_api/config/config.yaml b/projects/web_api/web_api/config/config.yaml index 1bdb5cf3..d2ca3577 100644 --- a/projects/web_api/web_api/config/config.yaml +++ b/projects/web_api/web_api/config/config.yaml @@ -11,6 +11,8 @@ BaseConfig: &base JWT_ACCESS_TOKEN_EXPIRES: 3600 PDF_UPLOAD_FOLDER: "upload_pdf" PDF_ANALYSIS_FOLDER: "analysis_pdf" + # 前端项目打包的路径 + REACT_APP_DIST: "../../web/dist/" # 开发配置 DevelopmentConfig: diff --git a/projects/web_api/web_api/config/mineru_web.db b/projects/web_api/web_api/config/mineru_web.db index 653cdad4a3e4dcd2afdf891a121c0374dc96ccab..fcac36060408e8c406a56b338c239853183f09b5 100644 GIT binary patch delta 36 jcmZo@P-;k+ASJ}W#K6G748$JnURbKfGiAX9BM}5T3X0vBQq^&rj1t8THMP_OD)AOps%3c|J>{D$K7wFhX=sT 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