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

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

2012-04-25

arxiv.org/abs/1204.5696v1

IAU Symp.282:470-471,2012

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

2 pages, 1 figure, presented at the IAU Symposium 282 "From Interacting Binaries to Exoplanets: Essential Modeling Tools", Tat

Scientific paper

10.1017/S1743921311028134

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 ~ 250kK), 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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