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Article: The carbon-rich proto planetary nebula IRAS 22272 + 5435

TitleThe carbon-rich proto planetary nebula IRAS 22272 + 5435
Authors
KeywordsInfrared: Sources
Nebulae: Individual (Iras 22272 + 5435)
Nebulae: Planetary
Stars: Circumstellar Shells
Issue Date1991
PublisherInstitute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637X
Citation
The Astrophysical Journal, 1991, v. 371 n. 2, p. 631-635 How to Cite?
AbstractGround-based photometry and spectroscopy is presented for IRAS 22272 + 5435, a 9th mag star with a large infrared excess. The flux distribution is "double-peaked," with a visible and near-infrared component due to the reddened photosphere and a far-infrared component presumably due to a detached dust shell. About equal amounts of energy are detected from each. The spectrum is that of a peculiar G supergiant, Gp Ia. In addition, strong molecular bands of C3 and C2 are observed. The flux distribution is modeled and, together with published molecular-line radio observations, allows the determination of basic parameters of the central star and the dust shell. The source has the characteristics one would expect of a proto-planetary nebula, an object in transition from the asymptotic giant branch to the planetary nebula phase.
Persistent Identifierhttp://hdl.handle.net/10722/179669
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266

 

DC FieldValueLanguage
dc.contributor.authorHrivnak, BJen_US
dc.contributor.authorKwok, Sen_US
dc.date.accessioned2012-12-19T10:02:43Z-
dc.date.available2012-12-19T10:02:43Z-
dc.date.issued1991en_US
dc.identifier.citationThe Astrophysical Journal, 1991, v. 371 n. 2, p. 631-635en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/10722/179669-
dc.description.abstractGround-based photometry and spectroscopy is presented for IRAS 22272 + 5435, a 9th mag star with a large infrared excess. The flux distribution is "double-peaked," with a visible and near-infrared component due to the reddened photosphere and a far-infrared component presumably due to a detached dust shell. About equal amounts of energy are detected from each. The spectrum is that of a peculiar G supergiant, Gp Ia. In addition, strong molecular bands of C3 and C2 are observed. The flux distribution is modeled and, together with published molecular-line radio observations, allows the determination of basic parameters of the central star and the dust shell. The source has the characteristics one would expect of a proto-planetary nebula, an object in transition from the 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.subjectInfrared: Sourcesen_US
dc.subjectNebulae: Individual (Iras 22272 + 5435)en_US
dc.subjectNebulae: Planetaryen_US
dc.subjectStars: Circumstellar Shellsen_US
dc.titleThe carbon-rich proto planetary nebula IRAS 22272 + 5435en_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.doi10.1086/169928-
dc.identifier.scopuseid_2-s2.0-0040622186en_US
dc.identifier.volume371en_US
dc.identifier.issue2en_US
dc.identifier.spage631en_US
dc.identifier.epage635en_US
dc.publisher.placeUnited Kingdomen_US
dc.identifier.scopusauthoridHrivnak, BJ=35613962100en_US
dc.identifier.scopusauthoridKwok, S=22980498300en_US

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