{
  "id": "1011.0731",
  "version": "v1",
  "published": "2010-11-02T20:00:03.000Z",
  "updated": "2010-11-02T20:00:03.000Z",
  "title": "Using the X-ray Morphologies of Young Supernova Remnants to Constrain Explosion Type, Ejecta Distribution, and Chemical Mixing",
  "authors": [
    "Laura A. Lopez",
    "Enrico Ramirez-Ruiz",
    "Daniela Huppenkothen",
    "Carles Badenes",
    "David Pooley"
  ],
  "comment": "21 pages, 17 figures, submitted to ApJ; for full resolution figures, see http://astro.ucsc.edu/~lopez/lines.html",
  "categories": [
    "astro-ph.HE"
  ],
  "abstract": "Supernova remnants (SNRs) are a complex class of sources, and their heterogeneous nature has hindered the characterization of their general observational properties. To overcome this challenge, we use statistical tools to analyze the Chandra X-ray images of Galactic and Large Magellanic Cloud SNRs. We apply two techniques, a power-ratio method (a multipole expansion) and wavelet-transform analysis, to measure the global and local morphological properties of the X-ray line and thermal emission in twenty-four SNRs. We find that Type Ia SNRs have statistically more spherical and mirror symmetric thermal X-ray emission than core-collapse (CC) SNRs. The ability to type SNRs based on thermal emission morphology alone enables, for the first time, the typing of SNRs with weak X-ray lines or with low-resolution spectra. We identify one source, SNR G344.7-0.1, as originating from a CC explosion that was previously unknown, and we confirm the tentative Type Ia classifications of G337.2-0.7 and G272.2-3.2. Although the global morphology is indicative of the explosion type, the relative morphology of the X-ray line emission within SNRs is not: all sources in our sample have well-mixed ejecta, irrespective of stellar origin. In particular, we find that 90% of the bright metal-line emitting substructures are spatially coincident and have similar scales, even if the metals arise from different burning processes. Moreover, the overall X-ray line morphologies within each SNR are the same, with <6% differences. These findings reinforce that hydrodynamical instabilities can efficiently mix ejecta in Type Ia and CC SNRs. The only exception is W49B, which is likely from its jet-driven/bipolar SN explosion. Finally, we describe observational constraints that can be used to test hydrodynamical models of SNR evolution; notably, the filling factor of X-ray emission decreases with SNR age.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2010-11-02T20:00:03.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "young supernova remnants",
      "constrain explosion type",
      "x-ray line",
      "x-ray morphologies",
      "morphology"
    ],
    "tags": [
      "journal article"
    ],
    "publication": {
      "doi": "10.1088/0004-637X/732/2/114",
      "journal": "The Astrophysical Journal",
      "year": 2011,
      "month": "May",
      "volume": 732,
      "number": 2,
      "pages": 114
    },
    "note": {
      "typesetting": "TeX",
      "pages": 21,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 875468,
      "adsabs": "2011ApJ...732..114L"
    }
  }
}