Spectroscopic binaries in planetary nebulae

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

Abstract

It is already known that about 10% of central stars of planetary nebulae (PNe) are very short-period binaries (hours to days), which are detected through photometric variations. These must have been formed through common-envelope interactions in initially wide binaries, accompanied by ejection of the envelope and its subsequent photoionization as a PN. Radial-velocity observations by ourselves and others are now suggesting that an even larger fraction of planetary nuclei may be spectroscopic binaries, making the total binary fraction very large. However, we have not as yet been able to rule out the possibility that the apparent velocity changes are actually due to stellar-wind variations. Pending follow-up spectroscopic observations with large telescopes, it presently appears plausible that binary-star ejection is the major formation channel for planetary nebulae.

Original languageEnglish (US)
Title of host publicationPLANETARY NEBULAE AS ASTRONOMICAL TOOLS
Subtitle of host publicationInternational Conference on Planetary Nebulae as Astronomical Tools
Pages165-168
Number of pages4
DOIs
StatePublished - Nov 28 2005
EventInternational Conference on Planetary Nebulae as Astronomical Tools - Gdansk, Poland
Duration: Jun 28 2005Jul 2 2005

Publication series

NameAIP Conference Proceedings
Volume804
ISSN (Print)0094-243X
ISSN (Electronic)1551-7616

Other

OtherInternational Conference on Planetary Nebulae as Astronomical Tools
CountryPoland
CityGdansk
Period6/28/057/2/05

All Science Journal Classification (ASJC) codes

  • Physics and Astronomy(all)

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