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A Search for Type Ia Supernova Progenitors: the Central Stars of the Planetary Nebulae NGC 2392 and NGC 6026

Published online by Cambridge University Press:  17 January 2013

A. Danehkar ,
D. J. Frew ,
O. De Marco  and
Q. A. Parker
A. Danehkar
Affiliation:
Department of Physics and Astronomy, Macquarie University, Sydney, NSW 2109, Australia
D. J. Frew
Affiliation:
Department of Physics and Astronomy, Macquarie University, Sydney, NSW 2109, Australia
O. De Marco
Affiliation:
Department of Physics and Astronomy, Macquarie University, Sydney, NSW 2109, Australia
Q. A. Parker
Affiliation:
Department of Physics and Astronomy, Macquarie University, Sydney, NSW 2109, Australia Australian Astronomical Observatory, PO Box 296, Epping, NSW 1710, Australia email: ashkbiz.danehkar@mq.edu.au; david.frew@mq.edu.au
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Abstract

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We use photoionization modeling to assess the binary nature of the central stars of NGC 2392 and NGC 6026. If they are close binaries, they are potential Type Ia supernovae (SNe Ia) progenitors if the total mass exceeds the Chandrasekhar limit. We show that the nucleus of NGC 2392 likely has a hot, massive (≃1 M⊙) white dwarf companion, and a total mass of ~1.6 M⊙, making it an especially interesting system. The binary mass in NGC 6026 is less, ~1.1 M⊙. Even though its orbital period is short, it is not considered to be an SNe~Ia progenitor.

Keywords

planetary nebulae: individual (NGC 2392 & NGC 6026) — supernovae: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Issue S281: Binary Paths to Type Ia Supernovae Explosions , July 2011 , pp. 221 - 222
Copyright
Copyright © International Astronomical Union 2013

References

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