Theoretical expressions for evolutionary period changes in non-radially pulsating stars

Details Theoretical expressions for evolutionary period changes in non-radially pulsating stars Theoretical expressions for evolutionary period changes in non-radially pulsating stars

Nov 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...186..170b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 186, no. 1-2, Nov. 1987, p. 170-176.

Astronomy and Astrophysics

Astrophysics

5

Radial Distribution, Stellar Evolution, Stellar Oscillations, Variable Stars, Vibration Mode, Density Distribution, Isentropic Processes, Kelvin-Helmholtz Instability, Stellar Mass

Scientific paper

The two-time-variable approach is used to study the equations governing linear pulsations, radial or non-radial, of a star evolving on its Helmholtz-Kelvin time scale. It is assumed that the isentropic approximation of the period of the pulsation mode considered is much shorter than the star's Helmholtz-Kelvin time scale. An integral expression for the rate of evolutionary change of the isentropic approximation of the pulsation period is derived and is shown to be determined by the isentropic approximation of the eigenfunctions and by the rates of change of three properties of the mass layers inside the evolving star: the radial distance to the center, the isentropic sound velocity, and the density. A decrease or an increase of the isentropic sound velocity in a mass layer contributes to an increase or a decrease, respectively, of the period. A tentative approximation for the rates of evolutionary change of the isentropic approximations of periods of high-order non-radial g-modes is derived under the restriction that the region of the star that predominates in determining these periods is not located close to the surface.

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