CMR exploration: I. Filament structure with synthetic observations
In this paper, we carry out a pilot parameter exploration for the collision-induced magnetic reconnection (CMR) mechanism that forms filamentary molecular clouds. Following Kong et al., we utilize Athena to model CMR in the context of resistive magnetohydrodynamics (MHD), considering the effect from...
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| Main Authors: | , , , , |
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| Format: | Article (Journal) |
| Language: | English |
| Published: |
2023 April 11
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| In: |
The astrophysical journal. Supplement series
Year: 2023, Volume: 265, Issue: 2, Pages: 1-24 |
| ISSN: | 1538-4365 |
| DOI: | 10.3847/1538-4365/acbfb0 |
| Online Access: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.3847/1538-4365/acbfb0 Verlag, lizenzpflichtig, Volltext: https://dx.doi.org/10.3847/1538-4365/acbfb0 
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| Author Notes: | Shuo Kong, Volker Ossenkopf-Okada, Héctor G. Arce, Ralf S. Klessen, and Duo Xu |
MARC
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| 520 | |a In this paper, we carry out a pilot parameter exploration for the collision-induced magnetic reconnection (CMR) mechanism that forms filamentary molecular clouds. Following Kong et al., we utilize Athena to model CMR in the context of resistive magnetohydrodynamics (MHD), considering the effect from seven physical conditions, including the ohmic resistivity (η), the magnetic field (B), the cloud density (ρ), the cloud radius R, the isothermal temperature T, the collision velocity v x , and the shear velocity v z . Compared to their fiducial model, we consider a higher and a lower value for each one of the seven parameters. We quantify the exploration results with five metrics, including the density probability distribution function (ρ-PDF), the filament morphology (250 μm dust emission), the B-ρ relation, the dominant fiber width, and the ringiness that describes the significance of the ringlike substructures. The exploration forms straight and curved CMR filaments with rich substructures that are highly variable in space and time. The variation translates to fluctuation in all five metrics, reflecting the chaotic nature of magnetic reconnection in CMR. A temporary B ∝ ρ relation is noticeable during the first 0.6 Myr. Overall, the exploration provides useful initial insights into the CMR mechanism. | ||
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