Filament formation through collision-induced magnetic reconnection (doi:10.7910/DVN/CXHWRR)

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Filament formation through collision-induced magnetic reconnection

doi:10.7910/DVN/CXHWRR

Harvard Dataverse

2021-06-20

3

Kong, Shuo, 2021, "Filament formation through collision-induced magnetic reconnection", https://doi.org/10.7910/DVN/CXHWRR, Harvard Dataverse, V3

Filament formation through collision-induced magnetic reconnection

doi:10.7910/DVN/CXHWRR

Kong, Shuo (The University of Arizona)

Harvard Dataverse

Kong, Shuo

Kong, Shuo

2021-06-20

https://doi.org/10.7910/DVN/CXHWRR

Astronomy and Astrophysics

Data and figure files for the simulations in Kong et al. (2021, ApJ, 906, 80) and Kong et al. (2023, ApJS, 265, 58).

<a href="http://creativecommons.org/licenses/by/4.0">CC BY 4.0</a>

@ARTICLE{2021ApJ...906...80K, author = {{Kong}, Shuo and {Ossenkopf-Okada}, Volker and {Arce}, H{\'e}ctor G. and {Bally}, John and {S{\'a}nchez-Monge}, {\'A}lvaro and {McGehee}, Peregrine and {Suri}, S{\"u}meyye and {Klessen}, Ralf S. and {Carpenter}, John M. and {Lis}, Dariusz C. and {Nakamura}, Fumitaka and {Schilke}, Peter and {Smith}, Rowan J. and {Mairs}, Steve and {Goodman}, Alyssa and {Maureira}, Mar{\'\i}a Jos{\'e}}, title = "{The CARMA-NRO Orion Survey: Filament Formation via Collision-induced Magnetic Reconnection{\textemdash}the Stick in Orion A}", journal = {\apj}, keywords = {Molecular clouds, Magnetic fields, Star formation, Interstellar filaments, Interstellar medium, Giant molecular clouds, Millimeter astronomy, Computational astronomy, Astrophysical fluid dynamics, Magnetohydrodynamical simulations, Observational astronomy, Theoretical models, 1072, 994, 1569, 842, 847, 653, 1061, 293, 101, 1966, 1145, 2107, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics}, year = 2021, month = jan, volume = {906}, number = {2}, eid = {80}, pages = {80}, doi = {10.3847/1538-4357/abc687}, archivePrefix = {arXiv}, eprint = {2011.00183}, primaryClass = {astro-ph.GA}, adsurl = {https://ui.adsabs.harvard.edu/abs/2021ApJ...906...80K}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }

10.3847/1538-4357/abc687

@ARTICLE{2021ApJ...906...80K, author = {{Kong}, Shuo and {Ossenkopf-Okada}, Volker and {Arce}, H{\'e}ctor G. and {Bally}, John and {S{\'a}nchez-Monge}, {\'A}lvaro and {McGehee}, Peregrine and {Suri}, S{\"u}meyye and {Klessen}, Ralf S. and {Carpenter}, John M. and {Lis}, Dariusz C. and {Nakamura}, Fumitaka and {Schilke}, Peter and {Smith}, Rowan J. and {Mairs}, Steve and {Goodman}, Alyssa and {Maureira}, Mar{\'\i}a Jos{\'e}}, title = "{The CARMA-NRO Orion Survey: Filament Formation via Collision-induced Magnetic Reconnection{\textemdash}the Stick in Orion A}", journal = {\apj}, keywords = {Molecular clouds, Magnetic fields, Star formation, Interstellar filaments, Interstellar medium, Giant molecular clouds, Millimeter astronomy, Computational astronomy, Astrophysical fluid dynamics, Magnetohydrodynamical simulations, Observational astronomy, Theoretical models, 1072, 994, 1569, 842, 847, 653, 1061, 293, 101, 1966, 1145, 2107, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics}, year = 2021, month = jan, volume = {906}, number = {2}, eid = {80}, pages = {80}, doi = {10.3847/1538-4357/abc687}, archivePrefix = {arXiv}, eprint = {2011.00183}, primaryClass = {astro-ph.GA}, adsurl = {https://ui.adsabs.harvard.edu/abs/2021ApJ...906...80K}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }

@ARTICLE{2023ApJS..265...58K, author = {{Kong}, Shuo and {Ossenkopf-Okada}, Volker and {Arce}, H{\'e}ctor G. and {Klessen}, Ralf S. and {Xu}, Duo}, title = "{CMR Exploration. I. Filament Structure with Synthetic Observations}", journal = {\apjs}, keywords = {Molecular clouds, Interstellar medium, Magnetic fields, Magnetohydrodynamical simulations, Radiative transfer simulations, Astronomical simulations, Interstellar filaments, Star formation, Star forming regions, Collapsing clouds, Dense interstellar clouds, Plasma astrophysics, 1072, 847, 994, 1966, 1967, 1857, 842, 1569, 1565, 267, 371, 1261, Astrophysics - Astrophysics of Galaxies, Physics - Plasma Physics}, year = 2023, month = apr, volume = {265}, number = {2}, eid = {58}, pages = {58}, doi = {10.3847/1538-4365/acbfb0}, archivePrefix = {arXiv}, eprint = {2302.08336}, primaryClass = {astro-ph.GA}, adsurl = {https://ui.adsabs.harvard.edu/abs/2023ApJS..265...58K}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }

10.3847/1538-4365/acbfb0

@ARTICLE{2023ApJS..265...58K, author = {{Kong}, Shuo and {Ossenkopf-Okada}, Volker and {Arce}, H{\'e}ctor G. and {Klessen}, Ralf S. and {Xu}, Duo}, title = "{CMR Exploration. I. Filament Structure with Synthetic Observations}", journal = {\apjs}, keywords = {Molecular clouds, Interstellar medium, Magnetic fields, Magnetohydrodynamical simulations, Radiative transfer simulations, Astronomical simulations, Interstellar filaments, Star formation, Star forming regions, Collapsing clouds, Dense interstellar clouds, Plasma astrophysics, 1072, 847, 994, 1966, 1967, 1857, 842, 1569, 1565, 267, 371, 1261, Astrophysics - Astrophysics of Galaxies, Physics - Plasma Physics}, year = 2023, month = apr, volume = {265}, number = {2}, eid = {58}, pages = {58}, doi = {10.3847/1538-4365/acbfb0}, archivePrefix = {arXiv}, eprint = {2302.08336}, primaryClass = {astro-ph.GA}, adsurl = {https://ui.adsabs.harvard.edu/abs/2023ApJS..265...58K}, adsnote = {Provided by the SAO/NASA Astrophysics Data System} }

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B_H_4.tgz

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Athena++ output files for the strong field model B_H (Model #4 in Table 1 of Kong et al. 2023)

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B_L_3.tgz

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Athena++ output files for the weak field model B_L (Model #3 in Table 1 of Kong et al. 2023)

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CMRfield.mpg

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A movie showing the filament formation via CMR. The simulation data is from the fiducial model from Kong et al. (2021, ApJ, 906, 80). Gas with densities above rho=1 (840 cm-3) is volume rendered so we see the dense gas in the collision midplane. The streamlines show magnetic fields. The random seeding is between x=-0.08 and x=0.08 (pc). The movie shows the reconnection of field lines around the imaginary pancake that would form from the collision of two spheres. The pancake is encircled by the field loops and pinched (due to magnetic tension) toward the central axis where the filament forms. As the collision continues along x-axis, more dense gas forms in the pancake (y-z plane or the collision midplane) which is continuously transported to the central filament. At the end, helical fields wrap around the filament with confining surface pressure. Formation of dense cores and stars shall follow in the filament.

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eta_H_2.tgz

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Athena++ output files for the high-resistivity model eta_H (Model #2 in Table 1 of Kong et al. 2023)

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eta_L_1.tgz

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Athena++ output files for the low-resistivity model eta_L (Model #1 in Table 1 of Kong et al. 2023)

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MRCOL_0.tgz

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Athena++ output files for the fiducial model MRCOL (Model #0 in Table 1 of Kong et al. 2023)

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R2_H_8.tgz

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Athena++ output files for the larger radius model R2_H (Model #8 in Table 1 of Kong et al. 2023)

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R2_L_7.tgz

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Athena++ output files for the smaller radius model R2_L (Model #7 in Table 1 of Kong et al. 2023)

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rho2_H_6.tgz

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Athena++ output files for the higher density model rho2_H (Model #6 in Table 1 of Kong et al. 2023)

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rho2_L_5.tgz

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Athena++ output files for the lower density model rho2_L (Model #5 in Table 1 of Kong et al. 2023)

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rotation_zoom2.gif

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3D volume rendering of the CMR-filament at different time steps and projections.

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T_H_10.tgz

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Athena++ output files for the higher temperature model T_H (Model #10 in Table 1 of Kong et al. 2023)

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T_L_9.tgz

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Athena++ output files for the lower temperature model T_L (Model #9 in Table 1 of Kong et al. 2023)

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vx_H_12.tgz

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Athena++ output files for the faster collision model vx_H (Model #12 in Table 1 of Kong et al. 2023)

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vx_L_11.tgz

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Athena++ output files for the slower collision model vx_L (Model #11 in Table 1 of Kong et al. 2023)

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vz_H_14.tgz

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Athena++ output files for the faster shear model vz_H (Model #14 in Table 1 of Kong et al. 2023)

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vz_L_13.tgz

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Athena++ output files for the slower shear model vz_L (Model #13 in Table 1 of Kong et al. 2023)

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