Solving the mode identification problem in asteroseismology of F stars observed with Kepler

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dc.creator White, Timothy R.
dc.creator Bedding, Timothy R.
dc.creator Gruberbauer, Michael
dc.creator Benomar, Othman
dc.creator Stello, Dennis
dc.creator Appourchaux, Thierry
dc.creator Chaplin, William J.
dc.creator Christensen-Dalsgaard, Jorgen
dc.creator Elsworth, Yvonne P.
dc.creator Garcia, Rafael A.
dc.date.accessioned 2018-04-17T16:24:17Z
dc.date.available 2018-04-17T16:24:17Z
dc.date.issued 2012-06-01
dc.identifier.issn 2041-8205
dc.identifier.uri http://library2.smu.ca/handle/01/27422
dc.description Publisher's Version/PDF
dc.description.abstract Asteroseismology of F-type stars has been hindered by an ambiguity in identification of their oscillation modes. The regular mode pattern that makes this task trivial in cooler stars is masked by increased line widths. The absolute mode frequencies, encapsulated in the asteroseismic variable ε, can help solve this impasse because the values of ε implied by the two possible mode identifications are distinct. We find that the correct ε can be deduced from the effective temperature and the line widths and we apply these methods to a sample of solar-like oscillators observed with Kepler. en_CA
dc.language.iso en en_CA
dc.publisher IOP Publishing Limited en_CA
dc.relation.uri https://dx.doi.org/10.1088/2041-8205/751/2/L36
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 F stars
dc.subject.lcsh Stellar oscillations
dc.subject.lcsh Astroseismology
dc.title Solving the mode identification problem in asteroseismology of F stars observed with Kepler en_CA
dc.type Text en_CA
dcterms.bibliographicCitation Astrophysical Journal Letters 751(2), L36. (2012) 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: https://dx.doi.org/10.1088/2041-8205/751/2/L36
 
 

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