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Conference Paper: Photoionization models of the Eskimo nebula: Evidence for a binary central star?

TitlePhotoionization models of the Eskimo nebula: Evidence for a binary central star?
Authors
Danehkar, AshkbizFrew, David J.Parker, Quentin A.De Marco, Orsola
Keywordsphotoionization codes
shock models
Planetary nebulae: individual (NGC 2392)
Issue Date2011
Citation
Proceedings of the International Astronomical Union, 2011, v. 7, n. S282, p. 470-471 How to Cite?
DOI: http://dx.doi.org/10.1017/S1743921311028134
AbstractThe 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.
Persistent Identifierhttp://hdl.handle.net/10722/208985
ISSN
1743-9213
2020 SCImago Journal Rankings: 0.124
ISI Accession Number ID
WOS:000309244400137

 

DC FieldValueLanguage
dc.contributor.authorDanehkar, Ashkbiz-
dc.contributor.authorFrew, David J.-
dc.contributor.authorParker, Quentin A.-
dc.contributor.authorDe Marco, Orsola-
dc.date.accessioned2015-03-23T02:02:28Z-
dc.date.available2015-03-23T02:02:28Z-
dc.date.issued2011-
dc.identifier.citationProceedings of the International Astronomical Union, 2011, v. 7, n. S282, p. 470-471-
dc.identifier.issn1743-9213-
dc.identifier.urihttp://hdl.handle.net/10722/208985-
dc.description.abstractThe 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.-
dc.languageeng-
dc.relation.ispartofProceedings of the International Astronomical Union-
dc.subjectphotoionization codes-
dc.subjectshock models-
dc.subjectPlanetary nebulae: individual (NGC 2392)-
dc.titlePhotoionization models of the Eskimo nebula: Evidence for a binary central star?-
dc.typeConference_Paper-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1017/S1743921311028134-
dc.identifier.scopuseid_2-s2.0-84887333568-
dc.identifier.volume7-
dc.identifier.issueS282-
dc.identifier.spage470-
dc.identifier.epage471-
dc.identifier.eissn1743-9221-
dc.identifier.isiWOS:000309244400137-
dc.identifier.issnl1743-9213-

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