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Conference Paper: Planetary nebulae: Getting closer to an unbiased binary fraction

TitlePlanetary nebulae: Getting closer to an unbiased binary fraction
Authors
Douchin, DDe, MOJacoby, GHHillwig, TCFrew, DJBojicic, IJasniewicz, GParker, QAde Laverny, PNardetto, NSamadi, RValls-Gabaud, DWozniak, H
Editors
Editor(s):Boissier, S.
KeywordsISM: planetary nebulae: general
Stars: binaries: general
Stars: evolution
Infrared: stars
Issue Date2012
Citation
SF2A-2012: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics, December 1, 2012, p. 325-327 How to Cite?
AbstractWhy 80% of planetary nebulae are not spherical is not yet understood. The Binary Hypothesis states that a companion to the progenitor of the central star of a 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 nebula and to compare it with the main sequence population. Preliminary results from photometric variability and infrared excess techniques indicate that the binary fraction of central stars of planetary nebulae is higher than that of the putative main sequence progenitor population, implying that PNe could be preferentially formed via a binary channel. This article briefly reviews these results and future studies aiming to refine the binary fraction.
Persistent Identifierhttp://hdl.handle.net/10722/211307

 

DC FieldValueLanguage
dc.contributor.authorDouchin, D-
dc.contributor.authorDe, MO-
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.contributor.authorde Laverny, P-
dc.contributor.authorNardetto, N-
dc.contributor.authorSamadi, R-
dc.contributor.authorValls-Gabaud, D-
dc.contributor.authorWozniak, H-
dc.contributor.editorBoissier, S.-
dc.date.accessioned2015-07-08T03:24:28Z-
dc.date.available2015-07-08T03:24:28Z-
dc.date.issued2012-
dc.identifier.citationSF2A-2012: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics, December 1, 2012, p. 325-327-
dc.identifier.urihttp://hdl.handle.net/10722/211307-
dc.description.abstractWhy 80% of planetary nebulae are not spherical is not yet understood. The Binary Hypothesis states that a companion to the progenitor of the central star of a 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 nebula and to compare it with the main sequence population. Preliminary results from photometric variability and infrared excess techniques indicate that the binary fraction of central stars of planetary nebulae is higher than that of the putative main sequence progenitor population, implying that PNe could be preferentially formed via a binary channel. This article briefly reviews these results and future studies aiming to refine the binary fraction.-
dc.languageeng-
dc.relation.ispartofSF2A-2012: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics-
dc.subjectISM: planetary nebulae: general-
dc.subjectStars: binaries: general-
dc.subjectStars: evolution-
dc.subjectInfrared: stars-
dc.titlePlanetary nebulae: Getting closer to an unbiased binary fraction-
dc.typeConference_Paper-
dc.identifier.emailParker, QA: quentinp@hku.hk-
dc.identifier.authorityParker, QA=rp02017-
dc.identifier.spage325-
dc.identifier.epage327-

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