{
  "id": "2308.15831",
  "version": "v1",
  "published": "2023-08-30T08:11:54.000Z",
  "updated": "2023-08-30T08:11:54.000Z",
  "title": "A Dual-Zone Diffusion Model for High Energy Emissions of the Cygnus Cocoon",
  "authors": [
    "Shihong Zhan",
    "Wei Wang"
  ],
  "comment": "7 pages, 5 figures, MNRAS in press",
  "categories": [
    "astro-ph.HE"
  ],
  "abstract": "As one of the brightest galactic ${\\gamma}$-ray sources, the Cygnus Cocoon superbubble has been observed by many detectors, such as $Fermi$-LAT, ARGO, HAWC, and LHAASO. However, the origin of $\\gamma$-ray emission for the Cygnus Cocoon and the possible contribution to PeV cosmic rays are still under debate. The recent ultrahigh-energy $\\gamma$-ray observations by LHAASO up to 1.4 PeV towards the direction of the Cygnus Cocoon, as well as the neutrino event report of IceCube-201120A coming from the same direction, suggest that the Cygnus Cocoon may be one of the sources of high-energy cosmic rays in the Galaxy. In this work, we propose a dual-zone diffusion model for the Cygnus Cocoon: the cocoon region and surrounding interstellar medium (ISM). This scenario can account for the $\\gamma$-ray data from GeV to $\\sim$ 50 TeV and agree with the one sub-PeV neutrino event result from IceCube so far. Moreover, it predict a non-negligible contribution $\\gamma$-ray emission at hundreds TeV from the ISM surrounding the Cygnus Cocoon. This possible diffuse TeV-PeV gamma-ray features can be resolved by the future LHAASO observations.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2023-08-30T08:11:54.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "cygnus cocoon",
      "dual-zone diffusion model",
      "high energy emissions",
      "cosmic rays",
      "ray emission"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 7,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}