Supergiant pulsations with gray radiative transfer in the atmosphere

Details Supergiant pulsations with gray radiative transfer in the atmosphere Supergiant pulsations with gray radiative transfer in the atmosphere

Apr 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pasj...43..345z&link_type=abstract

Astronomical Society of Japan, Publications (ISSN 0004-6264), vol. 43, no. 2, 1991, p. 345-362.

Astronomy and Astrophysics

Astronomy

2

Radiative Transfer, Stellar Atmospheres, Stellar Oscillations, Supergiant Stars, Approximation, Eigenvalues, Hydrodynamic Equations, Limb Darkening, Stellar Models

Scientific paper

A method for the solution of gray radiative transfer in a spherical, pulsating atmosphere is described. This program is used to study the behavior of the emergent intensity and to compare the properties of pulsations in RT (radiative transfer) and diffusion approximations. It is found that the emergent intensity exhibits an oscillating peak in layers in which the light starts to pass through the atmosphere. The existence of this feature and its amplitude depend on the model and mode of pulsation; the peak is nearly absent in the Cepheid model, while it is present in supergiant and early-type star models. A comparison of the properties of the eigenfunctions shows that for the radial fundamental mode the perturbations are qualitatively, and in the Cepheid model quantitatively, similar in the RT and diffusion approximation. In the supergiant model it is found that the periods and stabilities of modes differ significantly from those obtained using a diffusion approximation. The RT models point to the sensitivity of the stability and pulsation periods of supergiants to the thermal boundary condition.

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