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Article: Binary planetary nebulae nuclei towards the Galactic bulge

TitleBinary planetary nebulae nuclei towards the Galactic bulge
Authors
KeywordsStars: binaries: close
ISM: planetary nebulae: general
Issue Date2009
Citation
Astronomy and Astrophysics, 2009, v. 505, n. 1, p. 249-263 How to Cite?
AbstractConsiderable effort has been applied towards understanding the precise shaping mechanisms responsible for the diverse range of morphologies exhibited by planetary nebulae (PNe). At least 10-20% of PNe have central stars (CSPN) with a close binary companion thought responsible for heavily shaping the ejected PN during common-envelope (CE) evolution, however morphological studies of the few available examples found no clear distinction between PNe and post-CE PNe. The discovery of several new binary central stars (CSPN) from the OGLE-III photometric variability survey has significantly increased the number of post-CE PNe available for morphological analysis to 30 PNe. High quality Gemini South narrow-band images are presented for most of the OGLE sample, while some previously known post-CE PNe are reanalysed with images from the literature. Nearly 30% of nebulae have canonical bipolar morphologies, however this could be as high as 60% once inclination effects are incorporated with the aid of geometric models. This is the strongest observational evidence yet linking CE evolution to bipolar morphologies. A higher than average proportion of the sample shows low-ionisation knots, filaments or jets suggesting they have a binary origin. These features are also common in nebulae around emission-line nuclei which may be explained by speculative binary formation scenarios for H-deficient CSPN. © 2009 ESO.
Persistent Identifierhttp://hdl.handle.net/10722/208894
ISSN
2014 Impact Factor: 4.378
2015 SCImago Journal Rankings: 2.446

 

DC FieldValueLanguage
dc.contributor.authorMiszalski, Brent-
dc.contributor.authorAcker, Agnès-
dc.contributor.authorParker, Quentin A.-
dc.contributor.authorMoffat, Anthony F J-
dc.date.accessioned2015-03-23T02:02:05Z-
dc.date.available2015-03-23T02:02:05Z-
dc.date.issued2009-
dc.identifier.citationAstronomy and Astrophysics, 2009, v. 505, n. 1, p. 249-263-
dc.identifier.issn0004-6361-
dc.identifier.urihttp://hdl.handle.net/10722/208894-
dc.description.abstractConsiderable effort has been applied towards understanding the precise shaping mechanisms responsible for the diverse range of morphologies exhibited by planetary nebulae (PNe). At least 10-20% of PNe have central stars (CSPN) with a close binary companion thought responsible for heavily shaping the ejected PN during common-envelope (CE) evolution, however morphological studies of the few available examples found no clear distinction between PNe and post-CE PNe. The discovery of several new binary central stars (CSPN) from the OGLE-III photometric variability survey has significantly increased the number of post-CE PNe available for morphological analysis to 30 PNe. High quality Gemini South narrow-band images are presented for most of the OGLE sample, while some previously known post-CE PNe are reanalysed with images from the literature. Nearly 30% of nebulae have canonical bipolar morphologies, however this could be as high as 60% once inclination effects are incorporated with the aid of geometric models. This is the strongest observational evidence yet linking CE evolution to bipolar morphologies. A higher than average proportion of the sample shows low-ionisation knots, filaments or jets suggesting they have a binary origin. These features are also common in nebulae around emission-line nuclei which may be explained by speculative binary formation scenarios for H-deficient CSPN. © 2009 ESO.-
dc.languageeng-
dc.relation.ispartofAstronomy and Astrophysics-
dc.subjectStars: binaries: close-
dc.subjectISM: planetary nebulae: general-
dc.titleBinary planetary nebulae nuclei towards the Galactic bulge-
dc.typeArticle-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1051/0004-6361/200912176-
dc.identifier.scopuseid_2-s2.0-70349694257-
dc.identifier.volume505-
dc.identifier.issue1-
dc.identifier.spage249-
dc.identifier.epage263-
dc.identifier.eissn1432-0746-

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