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Conference Paper: 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
Douchin, DDe Marco, OJacoby, GHHillwig, TCFrew, DJBojicic, IJasniewicz, GParker, QAski, JStachowski, GMoskalik, PBajan, K
Editors
Editor(s):Krzesin
Issue Date2012
Citation
18th European White Dwarf Workshop, Krakow, Poland, 13-17 August 2012, p. 293-293 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/10722/211241

 

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.contributor.authorski, J-
dc.contributor.authorStachowski, G-
dc.contributor.authorMoskalik, P-
dc.contributor.authorBajan, K-
dc.contributor.editorKrzesin-
dc.date.accessioned2015-07-08T03:23:34Z-
dc.date.available2015-07-08T03:23:34Z-
dc.date.issued2012-
dc.identifier.citation18th European White Dwarf Workshop, Krakow, Poland, 13-17 August 2012, p. 293-293-
dc.identifier.urihttp://hdl.handle.net/10722/211241-
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.ispartof18th European White Dwarf Workshop.-
dc.titleTesting the Binary Hypothesis for the Formation and Shaping of Planetary Nebulae-
dc.typeConference_Paper-
dc.identifier.emailParker, QA: quentinp@hku.hk-
dc.identifier.authorityParker, QA=rp02017-
dc.identifier.volume469-
dc.identifier.spage293-
dc.identifier.epage293-

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