{
  "id": "2311.07717",
  "version": "v1",
  "published": "2023-11-13T19:57:59.000Z",
  "updated": "2023-11-13T19:57:59.000Z",
  "title": "Cooling and Instabilities in Colliding Radiative Flows with Toroidal Magnetic Fields",
  "authors": [
    "R. N. Markwick",
    "A. Frank",
    "E. G. Blackman",
    "J. Carroll-Nellenback",
    "S. V. Lebedev",
    "D. R. Russell",
    "J. W. D. Halliday",
    "L. G. Suttle",
    "P. M. Hartigan"
  ],
  "comment": "14 pages, 16 figures. Submitted to MNRAS",
  "categories": [
    "astro-ph.HE",
    "physics.plasm-ph"
  ],
  "abstract": "We report on the results of a simulation based study of colliding magnetized plasma flows. Our set-up mimics pulsed power laboratory astrophysical experiments but, with an appropriate frame change, are relevant to astrophysical jets with internal velocity variations. We track the evolution of the interaction region where the two flows collide. Cooling via radiative loses are included in the calculation. We systematically vary plasma beta ($\\beta_m$) in the flows, the strength of the cooling ($\\Lambda_0$) and the exponent ($\\alpha$) of temperature-dependence of the cooling function. We find that for strong magnetic fields a counter-propagating jet called a \"spine\" is driven by pressure from shocked toroidal fields. The spines eventually become unstable and break apart. We demonstrate how formation and evolution of the spines depends on initial flow parameters and provide a simple analytic model that captures the basic features of the flow.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2023-11-13T19:57:59.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "toroidal magnetic fields",
      "colliding radiative flows",
      "power laboratory astrophysical experiments",
      "pulsed power laboratory astrophysical",
      "set-up mimics pulsed power laboratory"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 14,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}