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Article: CO observations of candidates for carbon-rich asymptotic giant branch and post-asymptotic giant branch stars

TitleCO observations of candidates for carbon-rich asymptotic giant branch and post-asymptotic giant branch stars
Authors
KeywordsCircumstellar Matter
Infrared: Stars
Stars: Carbon
Stars: Post-Asymptotic Giant Branch
Issue Date1993
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637X
Citation
The Astrophysical Journal, 1993, v. 402 n. 1, p. 292-302 How to Cite?
AbstractCircumstellar CO emission has been detected in a number of featureless or weak SiC emission, low color temperature IRAS sources. The CO detections confirm the suggestion that these are either extreme carbon stars, carbon-rich proto-planetary nebulae (PPNs), or carbon-rich planetary nebulae (PNs). We find that the CO emission is relatively stronger for a given luminosity in post-AGB stars than AGB stars, suggesting a more efficient excitation mechanism is at work in the post-AGB phase. One probable post-AGB star was detected in HCN for the first time. The available HCN data suggest a rapid decline in HCN emission after the AGB. Molecular emission is shown to be a useful tracer of the evolution from asymptotic giant branch to the planetary nebula phase.
Persistent Identifierhttp://hdl.handle.net/10722/179677
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266

 

DC FieldValueLanguage
dc.contributor.authorVolk, Ken_US
dc.contributor.authorKwok, Sen_US
dc.contributor.authorWoodsworth, AWen_US
dc.date.accessioned2012-12-19T10:02:47Z-
dc.date.available2012-12-19T10:02:47Z-
dc.date.issued1993en_US
dc.identifier.citationThe Astrophysical Journal, 1993, v. 402 n. 1, p. 292-302en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/10722/179677-
dc.description.abstractCircumstellar CO emission has been detected in a number of featureless or weak SiC emission, low color temperature IRAS sources. The CO detections confirm the suggestion that these are either extreme carbon stars, carbon-rich proto-planetary nebulae (PPNs), or carbon-rich planetary nebulae (PNs). We find that the CO emission is relatively stronger for a given luminosity in post-AGB stars than AGB stars, suggesting a more efficient excitation mechanism is at work in the post-AGB phase. One probable post-AGB star was detected in HCN for the first time. The available HCN data suggest a rapid decline in HCN emission after the AGB. Molecular emission is shown to be a useful tracer of the evolution from asymptotic giant branch to the planetary nebula phase.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637Xen_US
dc.relation.ispartofThe Astrophysical Journalen_US
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.subjectCircumstellar Matteren_US
dc.subjectInfrared: Starsen_US
dc.subjectStars: Carbonen_US
dc.subjectStars: Post-Asymptotic Giant Branchen_US
dc.titleCO observations of candidates for carbon-rich asymptotic giant branch and post-asymptotic giant branch starsen_US
dc.typeArticleen_US
dc.identifier.emailKwok, S: deannote@hku.hken_US
dc.identifier.authorityKwok, S=rp00716en_US
dc.description.naturepublished_or_final_versionen_US
dc.identifier.doi10.1086/172132-
dc.identifier.scopuseid_2-s2.0-12044251136en_US
dc.identifier.volume402en_US
dc.identifier.issue1en_US
dc.identifier.spage292en_US
dc.identifier.epage302en_US
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridVolk, K=7006571965en_US
dc.identifier.scopusauthoridKwok, S=22980498300en_US
dc.identifier.scopusauthoridWoodsworth, AW=6602992543en_US

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