The structure of the thermal modes in pulsating stars

Details The structure of the thermal modes in pulsating stars The structure of the thermal modes in pulsating stars

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...303..740p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 303, April 15, 1986, p. 740-748.

Statistics

Computation

8

Computational Astrophysics, Eigenvectors, Stellar Oscillations, Thermal Diffusion, Variable Stars, Conductive Heat Transfer, Eigenvalues, Radiative Heat Transfer, Stellar Luminosity, Stellar Temperature

Scientific paper

The eigenvectors and eigenvalues of the linearized thermal diffusion operator are studied and their effect on the thermal structure of radial stellar pulsations is examined. It is shown on the basis of two specific cases that the difference between these eigenvectors may explain the lack of pulsational instability of radial modes in the Beta Cephei stars. A rigorous definition of the thermal response time of a model is attempted and the location of the transition from adiabatic to highly nonadiabatic motion is discussed.

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