Evolution, structure, and seismology of intermediate-mass stars

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dc.creator Guenther, David B.
dc.date.accessioned 2015-02-02T18:58:10Z
dc.date.available 2015-02-02T18:58:10Z
dc.date.issued 2002-04
dc.identifier.issn 0004-637X
dc.identifier.issn 1538-4357
dc.identifier.uri http://library2.smu.ca/xmlui/handle/01/25937
dc.description Publisher's version/PDF en_CA
dc.description.abstract The interior structure, the evolution, and the p-mode oscillation spectra of stellar models between 2.0 and 5 M[subscript circled dot] are presented. Interior details, including convective core and envelope growth and decay, the development of composition gradients, and the onset of hydrogen shell burning are shown to be testable by future asteroseismology observations. The stellar age and mass dependence of the large- and small-spacing oscillation frequencies are discussed. The dependencies of the structure and the oscillation spectra on composition and mixing length are also discussed. A new oscillation diagnostic for stellar mass is introduced. en_CA
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dc.language.iso en en_CA
dc.publisher American Astronomical Society en_CA
dc.relation.uri http://dx.doi.org/10.1086/339350
dc.rights Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user.
dc.subject.lcsh Stars -- Evolution
dc.subject.lcsh Stellar oscillations
dc.subject.lcsh Stars -- Structure
dc.title Evolution, structure, and seismology of intermediate-mass stars en_CA
dc.type Text en_CA
dcterms.bibliographicCitation Astrophysical Journal 569, 911-940. (2002) en_CA
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Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user.
 
Published Version: http://dx.doi.org/10.1086/339350
 
 

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