Photoionization models of the Eskimo nebula:evidence for a binary central star?

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 b...

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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.
Other Authors: Richards, Mercedes T., Hubeny, Ivan
Format: Article in Journal/Newspaper
Language:English
Published: 2011
Subjects:
Planetary nebulae: individual (NGC 2392)
photoionization codes
shock models
Hubble
eskimo*
Online Access:https://researchers.mq.edu.au/en/publications/dbe5600f-62f6-4005-8ffa-37f2b2b00fb4
https://doi.org/10.1017/S1743921311028134
http://www.scopus.com/inward/record.url?scp=84887333568&partnerID=8YFLogxK
Description
Summary: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.

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