Non-radial oscillations in rotating intermediate mass stars

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dc.contributor.advisor Deupree, Robert G. (Robert Gaston), 1946-
dc.contributor.author Lovekin, Catherine
dc.coverage.spatial Outer space
dc.date.accessioned 2010-08-27T16:28:26Z
dc.date.available 2010-08-27T16:28:26Z
dc.date.issued 2008
dc.identifier.uri http://library2.smu.ca/xmlui/handle/01/9023
dc.description ii [i.e. xii], 118 leaves : ill. ; 29 cm. en_CA
dc.description Includes bibliographical references (leaves 111-118).
dc.description Includes abstract.
dc.description.abstract In this work I investigate the influence of rotation on pulsation frequencies in upper main sequence stars. I use 2D stellar structure models and a 2D linear adiabatic pulsation code to calculate pulsation frequencies for both uniformly and differentially rotating 10 [Special characters omitted.] ZAMS models. Current techniques for these calculations often assume that the pulsation mode can be modelled using a single spherical harmonic and that the rotation rate is slow enough for second order perturbation theory approaches to be valid. These techniques require the rotation rate to be small enough to be considered a small linear perturbation. Using my 2D models, I am able to determine independent limits on the rotation rates for which these techniques are valid. These limits depend strongly on the mode and property in question, and range from 50-400 km sˉ¹. In general, uniform rotation decreases both the frequencies and the large separations, but produces increases in the small separations. In differentially rotating models, the frequencies may either increase or decrease, depending on the mode. Since these variations move in opposite directions, it may be possible to constrain the interior angular momentum distribution from stellar pulsations. Unfortunately, the differences are small, and the observational challenges may be insurmountable. Finally, I investigate how the distortion in the shape of the eigenfunction influences photometric mode identification techniques. Increasing rotation increases the variation in photometric mode identification as a function of inclination, with the result that it may be impossible to rule out certain modes. en_CA
dc.language.iso en en_CA
dc.publisher Halifax, N.S. : Saint Mary's University
dc.subject.lcc QB812
dc.subject.lcsh Stellar oscillations
dc.subject.lcsh Stars -- Rotation
dc.title Non-radial oscillations in rotating intermediate mass stars en_CA
dc.type Text en_CA
thesis.degree.name Doctor of Philosophy in Astronomy
thesis.degree.level Doctoral
thesis.degree.discipline Astronomy and Physics
thesis.degree.grantor Saint Mary's University (Halifax, N.S.)


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