On radiative and convective influences on stellar pulsational stability

Details On radiative and convective influences on stellar pulsational stability On radiative and convective influences on stellar pulsational stability

Dec 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988esasp.286...47b&link_type=abstract

In ESA, Seismology of the Sun and Sun-Like Stars p 47-52 (SEE N89-25819 19-92)

Physics

6

Cepheid Variables, Pulsed Radiation, Solar Activity, Stellar Envelopes, Stellar Radiation, Stellar Structure, Convection, Eddington Approximation, Radiative Heat Transfer, Reynolds Stress

Scientific paper

Gough's (1977) convection theory is applied to Cepheids and the Sun. It is shown that its inclusion may exert a stabilizing influence, particularly on stars on the cool side of the Cepheid instability strip. The role of Reynolds stress in stellar structure and stability is unclear. For solar acoustic modes, a modified version of the theory was applied to calculate pulsation growth rates within the Eddington approximation to radiative transfer. Results agree with previous calculations. When the calculation includes mixing length representations of the fluctuations of the convective heat flux and Reynolds stress, almost all of the modes are stabilized.

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