Estimating the binary fraction of planetary nebulae central stars

D. Douchin, O. De Marco, D. J. Frew, G. H. Jacoby, J. C. Passy, T. Hillwig, S. B. Howell, H. Bond, A. Peyaud, A. Zijlstra, R. Napiwotzki, G. Jasniewicz, Q. Parker

    Research output: Chapter in Book/Conference proceedingConference contributionpeer-review

    Abstract

    During the past 20 years, the idea that non-spherical planetary nebulae might need a binary or planetary interaction to be shaped was discussed by various authors. It is now generally agreed that the varied morphologies of planetary nebulae cannot be fully explained solely by single star evolution. Observationally, more binary central stars of planetary nebulae have been discovered, opening new possibilities to understand the connections between binarity and morphology. So far, ≃45 binary central stars of planetary nebulae have been detected, most being close systems detected via flux variability. In order to determine the PN binary fraction, one needs a method that can detect wider binaries. We present here recent results concentrating on binary infrared excess observations aimed at detecting binaries of any separation. © 2012 International Astronomical Union.
    Original languageEnglish
    Title of host publicationProceedings of the International Astronomical Union|Proc. Int. Astron. Union
    Pages346-347
    Number of pages1
    Volume7
    DOIs
    Publication statusPublished - Jul 2011

    Publication series

    NameIAU Symposium

    Keywords

    • binaries: general
    • planetary nebulae: general
    • stars: statistics
    • techniques: photometric
    • techniques: radial velocities

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