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, Ashkbiz, Frew, David J., Parker, Quentin A., De Marco, Orsola
Format: Conference Object
Language:English
Published: 2011
Subjects:
photoionization codes
Planetary nebulae: individual (NGC 2392)
shock models
Hubble
eskimo*
Online Access:https://doi.org/10.1017/S1743921311028134
http://hdl.handle.net/10722/208985
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. © International Astronomical Union 2012. link_to_subscribed_fulltext

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