Cloud-Cloud Collision: Formation of Hub-Filament Systems and Associated Gas Kinematics; Mass-collecting cone: A new signature of Cloud-Cloud Collision
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| Main Authors: | , , , , , , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866910564772478976 |
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| author | Maity, A. K. Inoue, T. Fukui, Y. Dewangan, L. K. Sano, H. Yamada, R. I. Tachihara, K. Bhadari, N. K. Jadhav, O. R. |
| author_facet | Maity, A. K. Inoue, T. Fukui, Y. Dewangan, L. K. Sano, H. Yamada, R. I. Tachihara, K. Bhadari, N. K. Jadhav, O. R. |
| contents | Massive star-forming regions (MSFRs) are commonly associated with hub-filament systems (HFSs) and sites of cloud-cloud collision (CCC). Recent observational studies of some MSFRs suggest a possible connection between CCC and the formation of HFSs. To understand this connection, we analyzed the magneto-hydrodynamic simulation data from Inoue et al. (2018). This simulation involves the collision of a spherical turbulent molecular cloud with a plane-parallel sea of dense molecular gas at a relative velocity of about 10 km/s. Following the collision, the turbulent and non-uniform cloud undergoes shock compression, rapidly developing filamentary structures within the compressed layer. We found that CCC can lead to the formation of HFSs, which is a combined effect of turbulence, shock compression, magnetic field, and gravity. The collision between the cloud components shapes the filaments into a cone and drives inward flows among them. These inward flows merge at the vertex of the cone, rapidly accumulating high-density gas, which can lead to the formation of massive star(s). The cone acts as a mass-collecting machine, involving a non-gravitational early process of filament formation, followed by gravitational gas attraction to finalize the HFS. The gas distribution in the position-velocity (PV) and position-position spaces highlights the challenges in detecting two cloud components and confirming their complementary distribution if the colliding clouds have a large size difference. However, such CCC events can be confirmed by the PV diagrams presenting gas flow toward the vertex of the cone, which hosts gravitationally collapsing high-density objects, and by the magnetic field morphology curved toward the direction of the collision. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2408_06826 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Cloud-Cloud Collision: Formation of Hub-Filament Systems and Associated Gas Kinematics; Mass-collecting cone: A new signature of Cloud-Cloud Collision Maity, A. K. Inoue, T. Fukui, Y. Dewangan, L. K. Sano, H. Yamada, R. I. Tachihara, K. Bhadari, N. K. Jadhav, O. R. Astrophysics of Galaxies Massive star-forming regions (MSFRs) are commonly associated with hub-filament systems (HFSs) and sites of cloud-cloud collision (CCC). Recent observational studies of some MSFRs suggest a possible connection between CCC and the formation of HFSs. To understand this connection, we analyzed the magneto-hydrodynamic simulation data from Inoue et al. (2018). This simulation involves the collision of a spherical turbulent molecular cloud with a plane-parallel sea of dense molecular gas at a relative velocity of about 10 km/s. Following the collision, the turbulent and non-uniform cloud undergoes shock compression, rapidly developing filamentary structures within the compressed layer. We found that CCC can lead to the formation of HFSs, which is a combined effect of turbulence, shock compression, magnetic field, and gravity. The collision between the cloud components shapes the filaments into a cone and drives inward flows among them. These inward flows merge at the vertex of the cone, rapidly accumulating high-density gas, which can lead to the formation of massive star(s). The cone acts as a mass-collecting machine, involving a non-gravitational early process of filament formation, followed by gravitational gas attraction to finalize the HFS. The gas distribution in the position-velocity (PV) and position-position spaces highlights the challenges in detecting two cloud components and confirming their complementary distribution if the colliding clouds have a large size difference. However, such CCC events can be confirmed by the PV diagrams presenting gas flow toward the vertex of the cone, which hosts gravitationally collapsing high-density objects, and by the magnetic field morphology curved toward the direction of the collision. |
| title | Cloud-Cloud Collision: Formation of Hub-Filament Systems and Associated Gas Kinematics; Mass-collecting cone: A new signature of Cloud-Cloud Collision |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2408.06826 |