{
  "id": "1408.0896",
  "version": "v2",
  "published": "2014-08-05T09:22:11.000Z",
  "updated": "2014-11-13T06:31:27.000Z",
  "title": "A method for computing synchrotron and inverse-Compton emission from hydrodynamic simulations of supernova remnants",
  "authors": [
    "M. Obergaulinger",
    "J. Ma. Chimeno",
    "P. Mimica",
    "M. A. Aloy",
    "A. Iyudin"
  ],
  "comment": "15 pages, 3 figures; accepted, HEDLA 2014 special issue of High Energy Density Physics",
  "categories": [
    "astro-ph.SR",
    "astro-ph.HE"
  ],
  "abstract": "The observational signature of supernova remnants (SNRs) is very complex, in terms of both their geometrical shape and their spectral properties, dominated by non-thermal synchrotron and inverse-Compton scattering. We propose a post-processing method to analyse the broad-band emission of SNRs based on three-dimensional hydrodynamical simulations. From the hydrodynamical data, we estimate the distribution of non-thermal electrons accelerated at the shock wave and follow the subsequent evolution as they lose or gain energy by adiabatic expansion or compression and emit energy by radiation. As a first test case, we use a simulation of a bipolar supernova expanding into a cloudy medium. We find that our method qualitatively reproduces the main observational features of typical SNRs and produces fluxes that agree with observations to within a factor of a few. allowing for further use in more extended sets of models.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2014-08-05T09:22:11.000Z",
      "abstract": "The observational signature of supernova remnants (SNRs) is very complex, in terms of both their geometrical shape and their spectral properties, dominated by non-thermal synchrotron and inverse-Compton scattering. We propose a post-processing method to analyse the broad-band emission of SNRs based on three-dimensional hydrodynamical simulations. From the hydrodynamical data, we estimate the distribution of non-thermal electrons accelerated at the shock wave and follow the subsequent evolution as they lose or gain energy by adiabatic expansion or compression and emit energy by radiation. As a first test case, we use a simulation of a bipolar supernova expanding into a cloudy medium. We find that our method qualitatively reproduces the main observational features of typical SNRs and produces fluxes of the right order of magnitude, allowing for further use in more extended sets of models.",
      "comment": "14 pages, 3 figures; submitted to the HEDLA 2014 special issue of High Energy Density Physics",
      "journal": null,
      "doi": null,
      "authors": [
        "M. Obergaulinger",
        "P. Mimica",
        "M. A. Aloy",
        "A. Iyudin"
      ]
    },
    {
      "version": "v2",
      "updated": "2014-11-13T06:31:27.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "supernova remnants",
      "hydrodynamic simulations",
      "inverse-compton emission",
      "computing synchrotron",
      "main observational features"
    ],
    "publication": {
      "doi": "10.1016/j.hedp.2014.11.004",
      "journal": "High Energy Density Physics",
      "year": 2015,
      "month": "Dec",
      "volume": 17,
      "pages": 92
    },
    "note": {
      "typesetting": "TeX",
      "pages": 15,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 1309856,
      "adsabs": "2015HEDP...17...92O"
    }
  }
}