{
  "id": "1503.05463",
  "version": "v1",
  "published": "2015-03-18T16:00:12.000Z",
  "updated": "2015-03-18T16:00:12.000Z",
  "title": "Numerical simulations of super-luminous supernovae of type IIn",
  "authors": [
    "Luc Dessart",
    "Edouard Audit",
    "D. John Hillier"
  ],
  "comment": "paper accepted to MNRAS",
  "categories": [
    "astro-ph.SR",
    "astro-ph.HE"
  ],
  "abstract": "We present numerical simulations that include 1-D Eulerian multi-group radiation-hydrodynamics, 1-D non-LTE radiative transfer, and 2-D polarised radiative transfer for super-luminous interacting supernovae (SNe). Our reference model is a ~10Msun inner shell with 10^51erg ramming into a ~3Msun cold outer shell (the circumstellar-medium, or CSM) that extends from 10^15cm to 2x10^16cm and moves at 100km/s. We discuss the light curve evolution, which cannot be captured adequately with a grey approach. In these interactions, the shock-crossing time through the optically-thick CSM is much longer than the photon diffusion time. Radiation is thus continuously leaking from the shock through the CSM, in disagreement with the shell-shocked model that is often invoked. Our spectra redden with time, with a peak distribution in the near-UV during the first month gradually shifting to the optical range over the following year. Initially Balmer lines exhibit a narrow line core and the broad line wings that are characteristic of electron scattering in the SNe IIn atmospheres (CSM). At later times they also exhibit a broad blue shifted component which arises from the cold dense shell. Our model results are broadly consistent with the bolometric light curve and spectral evolution observed for SN2010jl. Invoking a prolate pole-to-equator density ratio in the CSM, we can also reproduce the ~2% continuum polarisation, and line depolarisation, observed in SN2010jl. By varying the inner shell kinetic energy and the mass and extent of the outer shell, a large range of peak luminosities and durations, broadly compatible with super-luminous SNe IIn like 2010jl or 2006gy, can be produced.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2015-03-18T16:00:12.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "numerical simulations",
      "type iin",
      "super-luminous supernovae",
      "light curve",
      "sne iin"
    ],
    "publication": {
      "doi": "10.1093/mnras/stv609"
    },
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "inspire": 1353375
    }
  }
}