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Article: CO observations of candidates for carbon-rich asymptotic giant branch and post-asymptotic giant branch stars
Title | CO observations of candidates for carbon-rich asymptotic giant branch and post-asymptotic giant branch stars |
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Authors | |
Keywords | Circumstellar Matter Infrared: Stars Stars: Carbon Stars: Post-Asymptotic Giant Branch |
Issue Date | 1993 |
Publisher | Institute 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? |
Abstract | Circumstellar 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 Identifier | http://hdl.handle.net/10722/179677 |
ISSN | 2023 Impact Factor: 4.8 2023 SCImago Journal Rankings: 1.905 |
ISI Accession Number ID |
DC Field | Value | Language |
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dc.contributor.author | Volk, K | en_US |
dc.contributor.author | Kwok, S | en_US |
dc.contributor.author | Woodsworth, AW | en_US |
dc.date.accessioned | 2012-12-19T10:02:47Z | - |
dc.date.available | 2012-12-19T10:02:47Z | - |
dc.date.issued | 1993 | en_US |
dc.identifier.citation | The Astrophysical Journal, 1993, v. 402 n. 1, p. 292-302 | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://hdl.handle.net/10722/179677 | - |
dc.description.abstract | Circumstellar 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.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 | Circumstellar Matter | en_US |
dc.subject | Infrared: Stars | en_US |
dc.subject | Stars: Carbon | en_US |
dc.subject | Stars: Post-Asymptotic Giant Branch | en_US |
dc.title | CO observations of candidates for carbon-rich asymptotic giant branch and post-asymptotic giant branch stars | 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 | 10.1086/172132 | - |
dc.identifier.scopus | eid_2-s2.0-12044251136 | en_US |
dc.identifier.volume | 402 | en_US |
dc.identifier.issue | 1 | en_US |
dc.identifier.spage | 292 | en_US |
dc.identifier.epage | 302 | en_US |
dc.identifier.isi | WOS:A1993KD94400025 | - |
dc.publisher.place | United Kingdom | en_US |
dc.identifier.scopusauthorid | Volk, K=7006571965 | en_US |
dc.identifier.scopusauthorid | Kwok, S=22980498300 | en_US |
dc.identifier.scopusauthorid | Woodsworth, AW=6602992543 | en_US |
dc.identifier.issnl | 0004-637X | - |