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Photoionization Models of the Eskimo Nebula: Evidence for a Binary Central Star?

Published online by Cambridge University Press:  23 April 2012

A. Danehkar ,
D. J. Frew ,
Q. A. Parker  and
O. De Marco
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
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
O. De Marco
Affiliation:
Department of Physics and Astronomy, Macquarie University, Sydney, NSW 2109, Australia
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Abstract

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The ionizing star of the planetary nebula NGC 2392 is too cool to explain the high excitation of the nebular shell, and an additional ionizing source is necessary. We use photoionization modeling to estimate the temperature and luminosity of the putative companion. Our results show it is likely to be a very hot (Teff ≃ 250 kK), dense white dwarf. If the stars form a close binary, they may merge within a Hubble time, possibly producing a Type Ia supernova.

Keywords

Planetary nebulae: individual (NGC 2392); photoionization codes; shock models
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S282: From Interacting Binaries to Exoplanets: Essential Modeling Tools , July 2011 , pp. 470 - 471
Copyright
Copyright © International Astronomical Union 2012

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