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- W2016182012 abstract "Abstract The ratio, C, of the dynamical time-scale to the thermal time-scale of a star is small. This fact is used to develop an asymptotic theory of stellar pulsations, valid in the limit C → 0. The method is demonstrated in four planar models: a polytrope, a polytrope with an isothermal atmosphere, a layer containing a single ionization zone of finite thickness, and a layer in which there is an ionization front. In each case there is a thermal boundary layer associated with the oscillation. When it lies within the isothermal atmosphere of the second model, it is strongly destabilizing. If an ionization zone or front is to drive a layer towards instability, it must lie within the thermal boundary layer. The results for all four are compared with numerical work, and the agreement is shown to be qualitatively good. Only pulsations of infinitesimal amplitude are considered, except for the fourth model in which the so-called “saturation effect” is examined." @default.
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- W2016182012 title "The boundary layer method for pulsating stars" @default.
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- W2016182012 doi "https://doi.org/10.1080/03091927908244533" @default.
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