{
  "id": "1106.5711",
  "version": "v3",
  "published": "2011-06-28T15:55:03.000Z",
  "updated": "2012-05-21T11:52:15.000Z",
  "title": "Neutrinos from WIMP annihilation in the Sun : Implications of a self-consistent model of the Milky Way's dark matter halo",
  "authors": [
    "Susmita Kundu",
    "Pijushpani Bhattacharjee"
  ],
  "comment": "Replaced with revised version; Latest published results from Super-Kamiokande incorporated; quantitative limits on the branching fractions of various WIMP annihilation channels become more stringent by factors of 3 - 4; references added; overall conclusions unchanged; 17 pages, Latex, 6 Figures, accepted for publication in Phys. Rev. D",
  "journal": "Phys. Rev. D 85, 123533 (2012)",
  "doi": "10.1103/PhysRevD.85.123533",
  "categories": [
    "astro-ph.GA",
    "hep-ph"
  ],
  "abstract": "Upper limits on the spin-independent (SI) as well as spin-dependent (SD) elastic scattering cross sections of WIMPs with protons, imposed by the Super-Kamiokande (S-K) upper limit on the neutrino flux from WIMP annihilation in the Sun, and their compatibility with the \"DAMA-compatible\" regions of the WIMP parameter space within which the annual modulation signal observed by the DAMA/LIBRA experiment is compatible with the null results of other direct detection experiments, are studied within the frame work of a self-consistent model of the finite-size dark matter (DM) halo of the Galaxy, the parameters of which are determined by a fit to the rotation curve data of the Galaxy. We find that the S-K implied upper limits on the WIMP-proton elastic cross section as a function of WIMP mass impose stringent restrictions on the branching fractions of the various WIMP annihilation channels. For SI interaction, while the S-K upper limits are consistent with the DAMA-compatible region of the WIMP parameter space if the WIMPs annihilate dominantly to $\\bbarb$\\ and/or $\\cbarc$, portions of the DAMA-compatible region can be excluded if WIMP annihilations to $\\tautau$ and $\\nu\\anu$ occur at larger than ~ 10% and 0.1% levels, respectively. For SD interaction, the restrictions on the possible annihilation channels are much more stringent, essentially ruling out the DAMA-compatible region of the WIMP parameter space if the relatively low-mass ($\\sim$ 2 -- 20 GeV) WIMPs under consideration annihilate predominantly to any mixture of $\\bbarb$, \\ $\\cbarc$, \\ $\\tautau$, \\ and $\\nu\\anu$ final states.",
  "revisions": [
    {
      "version": "v3",
      "updated": "2012-05-21T11:52:15.000Z"
    }
  ],
  "analyses": {
    "subjects": [
      "95.35.+d"
    ],
    "keywords": [
      "milky ways dark matter halo",
      "wimp annihilation",
      "self-consistent model",
      "wimp parameter space",
      "mass impose stringent restrictions"
    ],
    "tags": [
      "journal article"
    ],
    "publication": {
      "publisher": "APS",
      "journal": "Physical Review D",
      "year": 2012,
      "month": "Jun",
      "volume": 85,
      "number": 12,
      "pages": 123533
    },
    "note": {
      "typesetting": "LaTeX",
      "pages": 17,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 916039,
      "adsabs": "2012PhRvD..85l3533K"
    }
  }
}