Theoretical velocity structure of long-period variable star photospheres

Details Theoretical velocity structure of long-period variable star photospheres Theoretical velocity structure of long-period variable star photospheres

May 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...229.1029h&link_type=abstract

Astrophysical Journal, Part 1, vol. 229, May 1, 1979, p. 1029-1045.

Other

93

Photosphere, Propagation Velocity, Shock Wave Propagation, Stellar Models, Supergiant Stars, Variable Stars, Absorption Spectra, Atmospheric Models, Boundary Conditions, Boundary Value Problems, Line Spectra, Pulsed Radiation, Stellar Atmospheres, Stellar Mass, Velocity Distribution

Scientific paper

Numerical models for shock waves propagating through atmospheres of cool supergiant stars for a grid of masses and surface gravities have been calculated by assuming spherical symmetry, isothermality, and a periodic piston boundary condition. The results of these models can be restated by using parameters derived in Willson and Hill (1976); the reparametrization allows the generalization of these results to arbitrary stellar masses and radii. Application of the theoretical generalization to a variety of observed properties of R Leonis and Omicron Ceti allows the selection of a limited range of probable masses and radii for these stars; a mass of approximately 0.8 to 1.5 solar masses and a radius of about (1.3 to 2) x 10 to the 13th cm for Omicron Cet and a mass of 1.8 to 4.0 solar masses and a radius of (1.7 to 2.5) x 10 to the 13th cm for R Leo. It is concluded that both stars are pulsating in the fundamental mode, with a pulsation constant Q of approximately 0.1 day.

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