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Conference Paper: Estimating the binary fraction of planetary nebulae central stars
Title | Estimating the binary fraction of planetary nebulae central stars |
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Authors | |
Keywords | techniques: photometric binaries: general planetary nebulae: general stars: statistics techniques: radial velocities |
Issue Date | 2011 |
Citation | Proceedings of the International Astronomical Union, 2011, v. 7, n. S283, p. 346-347 How to Cite? |
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. |
Persistent Identifier | http://hdl.handle.net/10722/208954 |
ISSN | 2023 SCImago Journal Rankings: 0.121 |
ISI Accession Number ID |
DC Field | Value | Language |
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dc.contributor.author | Douchin, Dimitri | - |
dc.contributor.author | De Marco, Orsola | - |
dc.contributor.author | Frew, David J. | - |
dc.contributor.author | Jacoby, George H. | - |
dc.contributor.author | Passy, Jean Claude | - |
dc.contributor.author | Hillwig, Todd C. | - |
dc.contributor.author | Howell, Steve B. | - |
dc.contributor.author | Bond, Howard E. | - |
dc.contributor.author | Peyaud, Alan E J | - |
dc.contributor.author | Zijlstra, Albert A. | - |
dc.contributor.author | Napiwotzki, Ralf | - |
dc.contributor.author | Jasniewicz, Gerard | - |
dc.contributor.author | Parker, Quentin A. | - |
dc.date.accessioned | 2015-03-23T02:02:21Z | - |
dc.date.available | 2015-03-23T02:02:21Z | - |
dc.date.issued | 2011 | - |
dc.identifier.citation | Proceedings of the International Astronomical Union, 2011, v. 7, n. S283, p. 346-347 | - |
dc.identifier.issn | 1743-9213 | - |
dc.identifier.uri | http://hdl.handle.net/10722/208954 | - |
dc.description.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. | - |
dc.language | eng | - |
dc.relation.ispartof | Proceedings of the International Astronomical Union | - |
dc.subject | techniques: photometric | - |
dc.subject | binaries: general | - |
dc.subject | planetary nebulae: general | - |
dc.subject | stars: statistics | - |
dc.subject | techniques: radial velocities | - |
dc.title | Estimating the binary fraction of planetary nebulae central stars | - |
dc.type | Conference_Paper | - |
dc.description.nature | link_to_subscribed_fulltext | - |
dc.identifier.doi | 10.1017/S1743921312011350 | - |
dc.identifier.scopus | eid_2-s2.0-84865770028 | - |
dc.identifier.volume | 7 | - |
dc.identifier.issue | S283 | - |
dc.identifier.spage | 346 | - |
dc.identifier.epage | 347 | - |
dc.identifier.eissn | 1743-9221 | - |
dc.identifier.isi | WOS:000309944800076 | - |
dc.identifier.issnl | 1743-9213 | - |