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Time-dependent radiative transfer calculations for supernovae

Authors

  • D. John Hillier,

    Corresponding author
    1. Department of Physics and Astronomy & Pittsburgh Particle Physics, Astrophysics, and Cosmology Center (PITT PACC), University of Pittsburgh, Pittsburgh, PA 15260, USA
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  • Luc Dessart

    1. Laboratoire d’Astrophysique de Marseille, Université Aix-Marseille & CNRS, UMR7326, 38 rue Frédéric Joliot-Curie, 13388 Marseille, France
    2. Theoretical Astrophysics, California Institute of Technology, MC 350-17, Pasadena, CA 91125, USA
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E-mail: hillier@pitt.edu

ABSTRACT

In previous papers we discussed results from fully time-dependent radiative transfer models for core-collapse supernova (SN) ejecta, including the Type II-peculiar SN 1987A, the more ‘generic’ SN II-Plateau, and more recently Type IIb/Ib/Ic SNe. Here we describe the modifications to our radiative modelling code, cmfgen, which allowed those studies to be undertaken. The changes allow for time-dependent radiative transfer of SN ejecta in homologous expansion. In the modelling we treat the entire SN ejecta, from the innermost layer that does not fall back on the compact remnant out to the progenitor surface layers. From our non-local thermodynamic equilibrium time-dependent line-blanketed synthetic spectra, we compute the bolometric and multiband light curves: light curves and spectra are thus calculated simultaneously using the same physical processes and numerics. These upgrades, in conjunction with our previous modifications which allow the solution of the time-dependent rate equations, will improve the modelling of SN spectra and light curves, and hence facilitate new insights into SN ejecta properties, the SN progenitors and the explosion mechanisms. cmfgen can now be applied to the modelling of all SN types.

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