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Article: Testing the Binary Hypothesis for the Formation and Shaping of Planetary Nebulae

TitleTesting the Binary Hypothesis for the Formation and Shaping of Planetary Nebulae
Authors
Keywordsplanetary nebulae
binaries
observations
Issue Date2013
Citation
Central European Astrophysical Bulletin, 2013, v. 37, p. 391-395 How to Cite?
AbstractThere is no quantitative theory to explain why a high 80% of all planetary nebulae are non-spherical. The Binary Hypothesis states that a companion to the progenitor of a central star of planetary nebula is required to shape the nebula and even for a planetary nebula to be formed at all. A way to test this hypothesis is to estimate the binary fraction of central stars of planetary nebulae and to compare it with that of the main sequence population. Preliminary results from photometric variability and the infrared excess techniques indicate that the binary fraction of central stars of planetary nebulae is higher than that of the main sequence, implying that PNe could preferentially form via a binary channel. This article briefly reviews these results and current studies aiming to refine the binary fraction.
Persistent Identifierhttp://hdl.handle.net/10722/211288
ISSN

 

DC FieldValueLanguage
dc.contributor.authorDouchin, D-
dc.contributor.authorDe Marco, O-
dc.contributor.authorJacoby, GH-
dc.contributor.authorHillwig, TC-
dc.contributor.authorFrew, DJ-
dc.contributor.authorBojicic, I-
dc.contributor.authorJasniewicz, G-
dc.contributor.authorParker, QA-
dc.date.accessioned2015-07-08T03:24:12Z-
dc.date.available2015-07-08T03:24:12Z-
dc.date.issued2013-
dc.identifier.citationCentral European Astrophysical Bulletin, 2013, v. 37, p. 391-395-
dc.identifier.issn1845-8319-
dc.identifier.urihttp://hdl.handle.net/10722/211288-
dc.description.abstractThere is no quantitative theory to explain why a high 80% of all planetary nebulae are non-spherical. The Binary Hypothesis states that a companion to the progenitor of a central star of planetary nebula is required to shape the nebula and even for a planetary nebula to be formed at all. A way to test this hypothesis is to estimate the binary fraction of central stars of planetary nebulae and to compare it with that of the main sequence population. Preliminary results from photometric variability and the infrared excess techniques indicate that the binary fraction of central stars of planetary nebulae is higher than that of the main sequence, implying that PNe could preferentially form via a binary channel. This article briefly reviews these results and current studies aiming to refine the binary fraction.-
dc.languageeng-
dc.relation.ispartofCentral European Astrophysical Bulletin-
dc.subjectplanetary nebulae-
dc.subjectbinaries-
dc.subjectobservations-
dc.titleTesting the Binary Hypothesis for the Formation and Shaping of Planetary Nebulae-
dc.typeArticle-
dc.identifier.emailParker, QA: quentinp@hku.hk-
dc.identifier.authorityParker, QA=rp02017-
dc.identifier.volume37-
dc.identifier.spage391-
dc.identifier.epage395-

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