{
  "id": "1712.04492",
  "version": "v1",
  "published": "2017-12-12T20:12:44.000Z",
  "updated": "2017-12-12T20:12:44.000Z",
  "title": "Super-luminous Type II supernovae powered by magnetars",
  "authors": [
    "Luc Dessart",
    "Edouard Audit"
  ],
  "comment": "submitted to A&A on 2 Nov 2017",
  "categories": [
    "astro-ph.HE",
    "astro-ph.SR"
  ],
  "abstract": "Magnetar power is believed to be at the origin of numerous super-luminous supernovae (SNe) of Type Ic, arising from compact, hydrogen-deficient, Wolf-Rayet type stars. Here, we investigate the properties that magnetar power would have on standard-energy SNe associated with 15-20Msun blue or red supergiant (BSG/RSG) stars. We use a combination of Eulerian grey radiation-hydrodynamics and non-LTE steady-state radiative transfer to study their dynamical, photometric, and spectroscopic properties. Adopting magnetar fields of 1, 3.5, 7 x 10^14G and rotational energies of 0.4, 1, and 3 x 10^51erg, we produce bolometric light curves with a broad maximum covering 50-150d and a magnitude of 10^43-10^44erg/s. The spectra at maximum light are analogous to those of standard SNe II-P but bluer. Although the magnetar energy is channelled roughly in equal proportion between SN kinetic energy and SN luminosity, the latter may be boosted by a factor 10-100 compared to a standard SN II. This influence breaks the observed relation between brightness and expansion rate of standard Type II SNe. Magnetar energy injection also delays recombination and may even cause re-ionization, with a reversal in photospheric temperature and velocity. Depositing the magnetar energy in a narrow mass shell at the ejecta base leads to the formation of a dense shell at a few 1000km/s, which causes a light-curve bump at the end of the photospheric phase. Depositing this energy over a broad range of mass in the inner ejecta, to mimic the effect of multi-dimensional fluid instabilities, prevents the formation of a dense shell and produces an earlier-rising and smoother light curve. The magnetar influence on the SN radiation is generally not visible prior to 20-30d, during which one may discern a BSG from a RSG progenitor. We propose a magnetar model for the super-luminous Type II SN OGLE-SN14-073.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2017-12-12T20:12:44.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "super-luminous type",
      "supernovae",
      "dense shell",
      "magnetar power",
      "produce bolometric light curves"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}