Photoionization models of the Eskimo nebula

evidence for a binary central star?

A. Danehkar, D. J. Frew, Q. A. Parker, O. De Marco

Research output: Chapter in Book/Report/Conference proceedingConference proceeding contribution

8 Citations (Scopus)

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 ≃ 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.

Original languageEnglish
Title of host publicationFrom Interacting Binaries to Exoplanets: Essential Modeling Tools
EditorsMercedes T. Richards, Ivan Hubeny
Place of PublicationCambridge; New York
PublisherCambridge University Press
Pages470-471
Number of pages2
Volume7
ISBN (Print)9781107019829
DOIs
Publication statusPublished - Jul 2011
EventIAU Symposium - Lima, Peru, Lima
Duration: 5 Jan 201114 Jan 2011

Publication series

NameProceedings of the International Astronomical Union
NumberS282
Volume7
ISSN (Print)17439213
ISSN (Electronic)17439221

Conference

ConferenceIAU Symposium
CityLima
Period5/01/1114/01/11

Keywords

  • Planetary nebulae: individual (NGC 2392)
  • photoionization codes
  • shock models

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    Danehkar, A., Frew, D. J., Parker, Q. A., & De Marco, O. (2011). Photoionization models of the Eskimo nebula: evidence for a binary central star? In M. T. Richards, & I. Hubeny (Eds.), From Interacting Binaries to Exoplanets: Essential Modeling Tools (Vol. 7, pp. 470-471). (Proceedings of the International Astronomical Union; Vol. 7, No. S282). Cambridge; New York: Cambridge University Press. https://doi.org/10.1017/S1743921311028134