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Double White Dwarf Merger Rates

Published online by Cambridge University Press:  17 January 2013

Silvia Toonen ,
Gijs Nelemans  and
Simon Portegies Zwart
Silvia Toonen
Affiliation:
Department of Astrophysics, IMAPP, Radboud University Nijmegen, P.O. Box 9010, NL-6500 GL, Nijmegen, the Netherlands email: silviato@astro.ru.nl
Gijs Nelemans
Affiliation:
Department of Astrophysics, IMAPP, Radboud University Nijmegen, P.O. Box 9010, NL-6500 GL, Nijmegen, the Netherlands email: silviato@astro.ru.nl
Simon Portegies Zwart
Affiliation:
Leiden Observatory, Leiden University, P.O. Box 9513, NL-2300 RA, Leiden, The Netherlands
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Abstract

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Type Ia supernovae (SNe Ia) are very successfully used as standard candles on cosmological distance scales, but so far the nature of the progenitor(s) is unclear. A possible scenario for SNe Ia are merging carbon/oxygen white dwarfs with a combined mass exceeding the Chandrasekhar mass. We determine the theoretical rates and delay time distribution of these mergers for two different common envelope prescriptions and metallicities. The shape of the delay time distributions is rather insensitive to the assumptions. The normalization is a factor ~3–13 too low compared to observations.

Keywords

stars: evolutionwhite dwarfs — binaries: close
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Issue S281: Binary Paths to Type Ia Supernovae Explosions , July 2011 , pp. 223 - 224
Copyright
Copyright © International Astronomical Union 2013

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