{
  "id": "2408.06826",
  "version": "v1",
  "published": "2024-08-13T11:38:11.000Z",
  "updated": "2024-08-13T11:38:11.000Z",
  "title": "Cloud-Cloud Collision: Formation of Hub-Filament Systems and Associated Gas Kinematics; Mass-collecting cone: A new signature of Cloud-Cloud Collision",
  "authors": [
    "A. K. Maity",
    "T. Inoue",
    "Y. Fukui",
    "L. K. Dewangan",
    "H. Sano",
    "R. I. Yamada",
    "K. Tachihara",
    "N. K. Bhadari",
    "O. R. Jadhav"
  ],
  "comment": "30 pages, 15 figures, 4 table, Accepted for publication in The Astrophysical Journal",
  "categories": [
    "astro-ph.GA"
  ],
  "abstract": "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.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2024-08-13T11:38:11.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "cloud-cloud collision",
      "associated gas kinematics",
      "hub-filament systems",
      "mass-collecting cone",
      "diagrams presenting gas flow"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 30,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}