A&A 476, 1133-1143 (2007)
DOI: 10.1051/0004-6361:20078438

Double-detonation supernovae of sub-Chandrasekhar mass white dwarfs

M. Fink, W. Hillebrandt, and F. K. Röpke

Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching, Germany
    e-mail: mfink@mpa-garching.mpg.de

(Received 7 August 2007 / Accepted 3 October 2007)

Abstract
Type Ia supernovae are believed to be white dwarfs disrupted by a thermonuclear explosion. Here we investigate the scenario in which a rather low-mass, carbon-oxygen (C + O) white dwarf accumulates helium on its surface in a sufficient amount for igniting a detonation in the helium shell before the Chandrasekhar mass is reached. In principle, this can happen on white dwarfs accreting from a non-degenerate companion or by merging a C + O white dwarf with a low-mass helium one. In this scenario, the helium detonation is thought to trigger a secondary detonation in the C + O core. It is therefore called the "double-detonation sub-Chandrasekhar" supernova model. By means of a set of numerical simulations, we investigate the robustness of this explosion mechanism for generic 1- models and analyze its observable predictions. Also a resolution dependence in numerical simulations is analyzed. Hydrodynamic simulations of the double-detonation sub-Chandrasekhar scenario are conducted in two and three spatial dimensions. The propagation of thermonuclear detonation fronts, both in helium and in the carbon-oxygen mixture, is computed by means of both a level-set function and a simplified description for nuclear reactions. The decision whether a secondary detonation is triggered in the white dwarf's core or not is made based on criteria given in the literature. In a parameter study involving different initial flame geometries for He-shell masses of 0.2 and 0.1  (and thus 0.8 and 0.9  of C + O), we find that a secondary detonation ignition is a very robust process. Converging shock waves originating from the detonation in the He shell generate the conditions for a detonation near the center of the white dwarf in most of the cases considered. Finally, we follow the complete evolution of three selected models with 0.2  of He through the C/O-detonation phase and obtain ⁵⁶Ni-masses of about 0.40 to 0.45 . Although we have not done a complete scan of the possible parameter space, our results show that sub-Chandrasekhar models are not good candidates for normal or sub-luminous type Ia supernovae. The chemical composition of the ejecta features significant amounts of ⁵⁶Ni in the outer layers at high expansion velocities, which is inconsistent with near-maximum spectra.

Key words: supernovae: general -- nuclear reactions, nucleosynthesis, abundances -- hydrodynamics -- methods: numerical

© ESO 2007

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