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Article: Effects of mass loss on the late stages of stellar evolution

TitleEffects of mass loss on the late stages of stellar evolution
Authors
Issue Date1987
PublisherElsevier BV. The Journal's web site is located at http://www.elsevier.com/locate/physrep
Citation
Physics Reports, 1987, v. 156 n. 3, p. 111-146 How to Cite?
AbstractAdvances in the infrared and radio observational techniques in the last decade have led to a revolution in our understanding of the late stages of stellar evolution. Intermediate (1-8 M⊙) mass stars are found to be undergoing rapid mass loss in the form of a stellar wind during the asymptotic-giant-branch after the exhaustion of helium burning in the core. Significant fraction of the original stellar mass can be lost in short time scales of < 106 yr. The ejected mass constitutes the major component of matter returned by stars to the interstellar medium. Since such material has been heavily nuclear processed, they also represent the dominant mechanism of chemical enrichment of the Galaxy. The high rate of mass loss implies that the majority of Population I stars end their evolution as planetary nebulae and white dwarfs rather than superovae and neutron stars. In this review, we summarize recent observational methods in the determination of the mass loss rate and the associated physical parameters of the stellar wind. Since the observed mass loss rate greatly exceeds the nuclear burning rate, we also discuss the theoretical models on how such mass loss affects the asymptotic giant branch evolution. A scenario is presented on how red giants evolve into planetary nebulae, a process which has been very poorly understood until recently. Conjectures on how the current evolutionary "missing link" - the proto-planetary nebulae - could be identified are also considered. © 1987.
Persistent Identifierhttp://hdl.handle.net/10722/179697
ISSN
2015 Impact Factor: 16.24
2015 SCImago Journal Rankings: 8.102

 

DC FieldValueLanguage
dc.contributor.authorKwok, Sen_US
dc.date.accessioned2012-12-19T10:02:54Z-
dc.date.available2012-12-19T10:02:54Z-
dc.date.issued1987en_US
dc.identifier.citationPhysics Reports, 1987, v. 156 n. 3, p. 111-146en_US
dc.identifier.issn0370-1573en_US
dc.identifier.urihttp://hdl.handle.net/10722/179697-
dc.description.abstractAdvances in the infrared and radio observational techniques in the last decade have led to a revolution in our understanding of the late stages of stellar evolution. Intermediate (1-8 M⊙) mass stars are found to be undergoing rapid mass loss in the form of a stellar wind during the asymptotic-giant-branch after the exhaustion of helium burning in the core. Significant fraction of the original stellar mass can be lost in short time scales of < 106 yr. The ejected mass constitutes the major component of matter returned by stars to the interstellar medium. Since such material has been heavily nuclear processed, they also represent the dominant mechanism of chemical enrichment of the Galaxy. The high rate of mass loss implies that the majority of Population I stars end their evolution as planetary nebulae and white dwarfs rather than superovae and neutron stars. In this review, we summarize recent observational methods in the determination of the mass loss rate and the associated physical parameters of the stellar wind. Since the observed mass loss rate greatly exceeds the nuclear burning rate, we also discuss the theoretical models on how such mass loss affects the asymptotic giant branch evolution. A scenario is presented on how red giants evolve into planetary nebulae, a process which has been very poorly understood until recently. Conjectures on how the current evolutionary "missing link" - the proto-planetary nebulae - could be identified are also considered. © 1987.en_US
dc.languageengen_US
dc.publisherElsevier BV. The Journal's web site is located at http://www.elsevier.com/locate/physrepen_US
dc.relation.ispartofPhysics Reportsen_US
dc.titleEffects of mass loss on the late stages of stellar evolutionen_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-s2.0-33645707427en_US
dc.identifier.volume156en_US
dc.identifier.issue3en_US
dc.identifier.spage111en_US
dc.identifier.epage146en_US
dc.publisher.placeNetherlandsen_US
dc.identifier.scopusauthoridKwok, S=22980498300en_US

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