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

Abstract 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 li...

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Bibliographic Details
Published in:Proceedings of the International Astronomical Union
Main Authors: Danehkar, A., Frew, D. J., Parker, Q. A., De Marco, O.
Format: Article in Journal/Newspaper
Language:English
Published: Cambridge University Press (CUP) 2011
Subjects:
Astronomy and Astrophysics
Space and Planetary Science
Hubble
eskimo*
Online Access:http://dx.doi.org/10.1017/s1743921311028134
https://www.cambridge.org/core/services/aop-cambridge-core/content/view/S1743921311028134
Description
Summary:Abstract 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 ( T eff ≃ 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.

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