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Properties of Carbon-Oxygen White Dwarf Merger Remnants

Published online by Cambridge University Press:  17 January 2013

Chenchong Zhu ,
Philip Chang ,
Marten van Kerkwijk  and
James Wadsley
Chenchong Zhu*
Affiliation:
Department of Astronomy & Astrophysics, University of Toronto, 50 St. George Street, Toronto, Ontario, Canada, M5S 3H4
Philip Chang
Affiliation:
Department of Physics, University of Wisconsin-Milwaukee, 1900 E Kenwood Blvd., Milwaukee, Wisconsin 53211, USA
Marten van Kerkwijk
Affiliation:
Department of Astronomy & Astrophysics, University of Toronto, 50 St. George Street, Toronto, Ontario, Canada, M5S 3H4
James Wadsley
Affiliation:
Department of Physics & Astronomy, ABB-241, McMaster University, 1280 Main St. W, Hamilton, Ontario, Canada, L8S 4M1
*
Correspondence email: cczhu@astro.utoronto.ca
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Abstract

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Recent studies have shown that for suitable initial conditions both super- and sub-Chandrasekhar mass carbon-oxygen white dwarf mergers produce explosions similar to observed SNe Ia. The question remains, however, how much fine tuning is necessary to produce these conditions. We performed a large set of SPH merger simulations, sweeping the possible parameter space. We find trends for merger remnant properties, and discuss how our results affect the viability of our recently proposed sub-Chandrasekhar merger channel for SNe Ia.

Keywords

stars: white dwarfssupernovae — binaries: close — methods: n-body simulations

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