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Article: The carbon-rich proto planetary nebula IRAS 22272 + 5435
Title | The carbon-rich proto planetary nebula IRAS 22272 + 5435 |
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Authors | |
Keywords | Infrared: Sources Nebulae: Individual (Iras 22272 + 5435) Nebulae: Planetary Stars: Circumstellar Shells |
Issue Date | 1991 |
Publisher | Institute 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? |
Abstract | Ground-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 Identifier | http://hdl.handle.net/10722/179669 |
ISSN | 2023 Impact Factor: 4.8 2023 SCImago Journal Rankings: 1.905 |
ISI Accession Number ID |
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Hrivnak, BJ | en_US |
dc.contributor.author | Kwok, S | en_US |
dc.date.accessioned | 2012-12-19T10:02:43Z | - |
dc.date.available | 2012-12-19T10:02:43Z | - |
dc.date.issued | 1991 | en_US |
dc.identifier.citation | The Astrophysical Journal, 1991, v. 371 n. 2, p. 631-635 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/10722/179669 | - |
dc.description.abstract | Ground-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.language | eng | en_US |
dc.publisher | Institute of Physics Publishing Ltd. The Journal's web site is located at http://iopscience.iop.org/0004-637X | en_US |
dc.relation.ispartof | The Astrophysical Journal | en_US |
dc.subject | Infrared: Sources | en_US |
dc.subject | Nebulae: Individual (Iras 22272 + 5435) | en_US |
dc.subject | Nebulae: Planetary | en_US |
dc.subject | Stars: Circumstellar Shells | en_US |
dc.title | The carbon-rich proto planetary nebula IRAS 22272 + 5435 | en_US |
dc.type | Article | en_US |
dc.identifier.email | Kwok, S: deannote@hku.hk | en_US |
dc.identifier.authority | Kwok, S=rp00716 | en_US |
dc.description.nature | published_or_final_version | en_US |
dc.identifier.doi | 10.1086/169928 | - |
dc.identifier.scopus | eid_2-s2.0-0040622186 | en_US |
dc.identifier.volume | 371 | en_US |
dc.identifier.issue | 2 | en_US |
dc.identifier.spage | 631 | en_US |
dc.identifier.epage | 635 | en_US |
dc.identifier.isi | WOS:A1991FF98300020 | - |
dc.publisher.place | United Kingdom | en_US |
dc.identifier.scopusauthorid | Hrivnak, BJ=35613962100 | en_US |
dc.identifier.scopusauthorid | Kwok, S=22980498300 | en_US |
dc.identifier.issnl | 0004-637X | - |