On the treatment of convection as a nonradial stellar pulsation

Details On the treatment of convection as a nonradial stellar pulsation On the treatment of convection as a nonradial stellar pulsation

Jun 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...198..419d&link_type=abstract

Astrophysical Journal, vol. 198, June 1, 1975, pt. 1, p. 419-423.

Statistics

Computation

8

A Stars, Cepheid Variables, Convective Heat Transfer, Stellar Structure, Amplitude Distribution Analysis, Astronomical Models, Giant Stars, Stellar Luminosity

Scientific paper

The problem of nonlinear, nonadiabatic, nonradial stellar pulsation has been examined by a computational approach. The difficulties of such an approach are discussed in detail, and the limitations of the present method of solution are listed. A test calculation with a particular RR Lyrae model pulsating in the fundamental mode reveals that convection is present in the second helium ionization zone only when the luminosity amplitude becomes large and even then is present during only part of the pulsation cycle. The convective motion, measured by the nonradial velocity component, grows during rising luminosity, reaches a maximum after maximum luminosity, and decays during the other parts of the cycle. The possible consequences of this phenomenon are briefly discussed.

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