{
  "id": "2203.01508",
  "version": "v1",
  "published": "2022-03-03T04:12:08.000Z",
  "updated": "2022-03-03T04:12:08.000Z",
  "title": "The Velocity Statistics of Turbulent Clouds in the Presence of Gravity, Magnetic fields, Radiation, and Outflow Feedback",
  "authors": [
    "Yue Hu",
    "Christoph Federrath",
    "Siyao Xu",
    "Sajay Sunny Mathew"
  ],
  "comment": "11 pages, 9 figures, submitted to MNRAS",
  "categories": [
    "astro-ph.GA"
  ],
  "abstract": "The interaction of turbulence, magnetic fields, self-gravity, and stellar feedback within molecular clouds is crucial for understanding star formation. We study the effects of self-gravity and outflow feedback on the properties of the turbulent velocity via the structure function over length scales from $\\sim$ 0.01 pc to 2 pc. We analyze a series of three-dimensional, magnetohydrodynamical (MHD) simulations of star cluster formation, including self-gravity, turbulence, magnetic fields, stellar radiative heating, and outflow feedback. We observe that self-gravity and protostellar outflows increase the velocity fluctuations over all length scales. In particular, outflows can amplify the velocity fluctuations by up to a factor of $\\sim$7 on scales $\\sim$ 0.01 - 0.2 pc and drive turbulence up to a scale of $\\sim$ 1 pc. The amplified velocity fluctuations provide more support against gravity and enhance fragmentation on small scales. The role of self-gravity is more significant on smaller dense clumps and it increases the fraction of the compressive velocity component up to a scale of $\\sim$ 0.2 pc. However, outflow feedback drives both solenoidal and compressive modes, but it induces a higher fraction of solenoidal modes relative to compressive modes. Thus, with outflows, the dense core ends up with a slightly higher fraction of solenoidal modes. We find that the compressible fraction is fairly constant with about 1/3 on scales $\\sim$ 0.1 - 0.2 pc. The combined effect of enhanced velocity dispersion and reduced compressive fraction contributes to a reduction in the star formation rate compared to when outflow feedback is not included.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2022-03-03T04:12:08.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "outflow feedback",
      "magnetic fields",
      "velocity statistics",
      "turbulent clouds",
      "velocity fluctuations"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 11,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}