Estimating the binary fraction of central stars of planetary nebulae using the infrared excess method

D. Douchin, O. De Marco, D. J. Frew, G. H. Jacoby, M. Fitzgerald, M. Moe, J. C. Passy, T. Hillwig, D. Harmer

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 nebulae whose shapes are not spherical or mildly elliptical, implying that many single post-AGB stars do not make a PN 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 that of the main sequence population. Preliminary results from the infrared excess technique indicate that the binary fraction of central stars of planetary nebula is higher than that of the main sequence, implying that PNe could preferentially form via a binary channel. I will present new results from a search of red and infrared flux excess in an extended sample of central stars of planetary nebula and compare the improved estimate of the PN binary fraction with that of main sequence stars.
Original languageEnglish
Title of host publicationAsymmetrical Planetary Nebulae VI
Subtitle of host publicationproceedings
Place of PublicationRiviera Maya, Mexico
PublisherProceedings of the Asymmetrical Planetary Nebulae VI conference
Number of pages18
Publication statusPublished - 2014
EventAsymmetrical Planetary Nebulae (6th : 2013) - Riviera Maya, Mexico
Duration: 4 Nov 20138 Nov 2013

Conference

ConferenceAsymmetrical Planetary Nebulae (6th : 2013)
CityRiviera Maya, Mexico
Period4/11/138/11/13

Keywords

  • stars: planetary nebulae
  • planetary nebulae: general

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    Douchin, D., De Marco, O., Frew, D. J., Jacoby, G. H., Fitzgerald, M., Moe, M., ... Harmer, D. (2014). Estimating the binary fraction of central stars of planetary nebulae using the infrared excess method. In Asymmetrical Planetary Nebulae VI: proceedings Riviera Maya, Mexico: Proceedings of the Asymmetrical Planetary Nebulae VI conference.