Photoionization models of the Eskimo nebula: evidence for a binary central star?
Ashkbiz Danehkar, David J. Frew, Quentin A. Parker, Orsola De Marco
TL;DR
This study uses photoionization models to investigate the Eskimo nebula's ionizing source, suggesting a hot white dwarf companion that could lead to a Type Ia supernova if in a close binary system.
Contribution
It provides evidence for a binary central star in the Eskimo nebula and estimates the companion's properties using photoionization modeling.
Findings
The ionizing star is too cool to explain nebular excitation.
The companion is likely a very hot white dwarf (~250,000K).
The binary system could merge and produce a Type Ia supernova.
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 (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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