Testing the binary hypothesis for the formation and shaping of planetary nebulae

D. Douchin*, O. De Marco, G. H. Jacoby, T. C. Hillwig, D. J. Frew, I. Bojicic, G. Jasniewicz, Q. A. Parker

*Corresponding author for this work

Research output: Chapter in Book/Report/Conference proceedingConference proceeding contribution

Abstract

There 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.

Original languageEnglish
Title of host publication18th European White Dwarf Workshop
Subtitle of host publicationproceedings of a conference held at the Pedagogical University of Cracow, Poland, 13-17 August 201
EditorsJ Krzesinski, G Stachowski, P Moskalik, K Bajan
Place of PublicationSan Francisco, CA
PublisherASTRONOMICAL SOC PACIFIC
Pages293-296
Number of pages4
ISBN (Print)9781583818206
Publication statusPublished - 2013
Event18th European White Dwarf Workshop, EUROWD12 - Krakow, Poland
Duration: 13 Aug 201217 Aug 2012

Publication series

NameAstronomical Society of the Pacific Conference Series
PublisherASTRONOMICAL SOC PACIFIC
Volume469

Conference

Conference18th European White Dwarf Workshop, EUROWD12
CountryPoland
CityKrakow
Period13/08/1217/08/12

Keywords

  • SOLAR-TYPE STARS
  • MULTIPLICITY
  • PROGENITORS
  • SAMPLE

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