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Article: Properties of OH/IR stars with IRAS LRS spectra

TitleProperties of OH/IR stars with IRAS LRS spectra
Authors
Keywords(Stars:) Circumstellar Matter
Astronomical Data Bases: Miscellaneous
Masers
Stars: Agb And Post-Agb
Issue Date2001
PublisherE D P Sciences. The Journal's web site is located at http://www.aanda.org
Citation
Astronomy And Astrophysics, 2001, v. 368 n. 3, p. 1006-1020 How to Cite?
Abstract1858 OH satellite line (1612 MHz) maser sources associated with the IRAS counterparts were assembled from the literature. Cross-correlation between collected OH/IR - IRAS sources and the recent catalogue of the IRAS LRS spectra (Kwok et al. 1997) allows us to subdivide 1024 of them (after excluding OH sources with uncertain IRAS associations) into 10 groups according to the Volk & Cohen (1989) classification scheme. We have found that sources with silicate emission form the largest group (about 57%), followed by the group with silicate absorption (only about 16%). For more sensitive individual OH maser surveys these numbers differentiate even more and the ratio between silicate emission and absorption sources reaches a value close to 6. Surprisingly, we found an association of OH maser emission with a small number of stars with carbon-rich atmospheres. The distribution of these subgroups of OH/IR stars in the IRAS colour-colour and the period-colour diagrams as well as histograms of some physical properties are presented. The galactic distribution of important parameters (periods, IRAS colours, expansion and stellar velocities) for different classes of OH/IR sources is analyzed from the point of view of the stars' evolutionary status. The correlations among the periods, colours, expansion and star velocities and the pumping efficiencies for selected subgroups of OH/IR stars are also investigated. These analyses allow us to demonstrate that a significant fraction of silicate emission group sources do not form an evolutionary sequence with the silicate absorption objects - as is suggested e.g. by the IRAS colour-colour diagram, but rather form a lower initial mass sequence, i.e. these sources will never develop sufficient mass loss to manifest silicate absorption.
Persistent Identifierhttp://hdl.handle.net/10722/179657
ISSN
2014 Impact Factor: 4.378
2015 SCImago Journal Rankings: 2.446

 

DC FieldValueLanguage
dc.contributor.authorChen, PSen_US
dc.contributor.authorSzczerba, Ren_US
dc.contributor.authorKwok, Sen_US
dc.contributor.authorVolk, Ken_US
dc.date.accessioned2012-12-19T10:02:17Z-
dc.date.available2012-12-19T10:02:17Z-
dc.date.issued2001en_US
dc.identifier.citationAstronomy And Astrophysics, 2001, v. 368 n. 3, p. 1006-1020en_US
dc.identifier.issn0004-6361en_US
dc.identifier.urihttp://hdl.handle.net/10722/179657-
dc.description.abstract1858 OH satellite line (1612 MHz) maser sources associated with the IRAS counterparts were assembled from the literature. Cross-correlation between collected OH/IR - IRAS sources and the recent catalogue of the IRAS LRS spectra (Kwok et al. 1997) allows us to subdivide 1024 of them (after excluding OH sources with uncertain IRAS associations) into 10 groups according to the Volk & Cohen (1989) classification scheme. We have found that sources with silicate emission form the largest group (about 57%), followed by the group with silicate absorption (only about 16%). For more sensitive individual OH maser surveys these numbers differentiate even more and the ratio between silicate emission and absorption sources reaches a value close to 6. Surprisingly, we found an association of OH maser emission with a small number of stars with carbon-rich atmospheres. The distribution of these subgroups of OH/IR stars in the IRAS colour-colour and the period-colour diagrams as well as histograms of some physical properties are presented. The galactic distribution of important parameters (periods, IRAS colours, expansion and stellar velocities) for different classes of OH/IR sources is analyzed from the point of view of the stars' evolutionary status. The correlations among the periods, colours, expansion and star velocities and the pumping efficiencies for selected subgroups of OH/IR stars are also investigated. These analyses allow us to demonstrate that a significant fraction of silicate emission group sources do not form an evolutionary sequence with the silicate absorption objects - as is suggested e.g. by the IRAS colour-colour diagram, but rather form a lower initial mass sequence, i.e. these sources will never develop sufficient mass loss to manifest silicate absorption.en_US
dc.languageengen_US
dc.publisherE D P Sciences. The Journal's web site is located at http://www.aanda.orgen_US
dc.relation.ispartofAstronomy and Astrophysicsen_US
dc.subject(Stars:) Circumstellar Matteren_US
dc.subjectAstronomical Data Bases: Miscellaneousen_US
dc.subjectMasersen_US
dc.subjectStars: Agb And Post-Agben_US
dc.titleProperties of OH/IR stars with IRAS LRS spectraen_US
dc.typeArticleen_US
dc.identifier.emailKwok, S: deannote@hku.hken_US
dc.identifier.authorityKwok, S=rp00716en_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.scopuseid_2-s2.0-0035264474en_US
dc.identifier.volume368en_US
dc.identifier.issue3en_US
dc.identifier.spage1006en_US
dc.identifier.epage1020en_US
dc.publisher.placeFranceen_US
dc.identifier.scopusauthoridChen, PS=7408354675en_US
dc.identifier.scopusauthoridSzczerba, R=7004424914en_US
dc.identifier.scopusauthoridKwok, S=22980498300en_US
dc.identifier.scopusauthoridVolk, K=7006571965en_US

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