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Conference Paper: Estimating the binary fraction of planetary nebulae central stars

TitleEstimating the binary fraction of planetary nebulae central stars
Authors
Keywordstechniques: photometric
binaries: general
planetary nebulae: general
stars: statistics
techniques: radial velocities
Issue Date2011
Citation
Proceedings of the International Astronomical Union, 2011, v. 7, n. S283, p. 346-347 How to Cite?
AbstractDuring the past 20 years, the idea that non-spherical planetary nebulae might need a binary or planetary interaction to be shaped was discussed by various authors. It is now generally agreed that the varied morphologies of planetary nebulae cannot be fully explained solely by single star evolution. Observationally, more binary central stars of planetary nebulae have been discovered, opening new possibilities to understand the connections between binarity and morphology. So far, ≃45 binary central stars of planetary nebulae have been detected, most being close systems detected via flux variability. In order to determine the PN binary fraction, one needs a method that can detect wider binaries. We present here recent results concentrating on binary infrared excess observations aimed at detecting binaries of any separation. © 2012 International Astronomical Union.
Persistent Identifierhttp://hdl.handle.net/10722/208954
ISSN
2015 SCImago Journal Rankings: 0.105

 

DC FieldValueLanguage
dc.contributor.authorDouchin, Dimitri-
dc.contributor.authorDe Marco, Orsola-
dc.contributor.authorFrew, David J.-
dc.contributor.authorJacoby, George H.-
dc.contributor.authorPassy, Jean Claude-
dc.contributor.authorHillwig, Todd C.-
dc.contributor.authorHowell, Steve B.-
dc.contributor.authorBond, Howard E.-
dc.contributor.authorPeyaud, Alan E J-
dc.contributor.authorZijlstra, Albert A.-
dc.contributor.authorNapiwotzki, Ralf-
dc.contributor.authorJasniewicz, Gerard-
dc.contributor.authorParker, Quentin A.-
dc.date.accessioned2015-03-23T02:02:21Z-
dc.date.available2015-03-23T02:02:21Z-
dc.date.issued2011-
dc.identifier.citationProceedings of the International Astronomical Union, 2011, v. 7, n. S283, p. 346-347-
dc.identifier.issn1743-9213-
dc.identifier.urihttp://hdl.handle.net/10722/208954-
dc.description.abstractDuring the past 20 years, the idea that non-spherical planetary nebulae might need a binary or planetary interaction to be shaped was discussed by various authors. It is now generally agreed that the varied morphologies of planetary nebulae cannot be fully explained solely by single star evolution. Observationally, more binary central stars of planetary nebulae have been discovered, opening new possibilities to understand the connections between binarity and morphology. So far, ≃45 binary central stars of planetary nebulae have been detected, most being close systems detected via flux variability. In order to determine the PN binary fraction, one needs a method that can detect wider binaries. We present here recent results concentrating on binary infrared excess observations aimed at detecting binaries of any separation. © 2012 International Astronomical Union.-
dc.languageeng-
dc.relation.ispartofProceedings of the International Astronomical Union-
dc.subjecttechniques: photometric-
dc.subjectbinaries: general-
dc.subjectplanetary nebulae: general-
dc.subjectstars: statistics-
dc.subjecttechniques: radial velocities-
dc.titleEstimating the binary fraction of planetary nebulae central stars-
dc.typeConference_Paper-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1017/S1743921312011350-
dc.identifier.scopuseid_2-s2.0-84865770028-
dc.identifier.volume7-
dc.identifier.issueS283-
dc.identifier.spage346-
dc.identifier.epage347-
dc.identifier.eissn1743-9221-

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