Shock phenomena in a hydrodynamic model of a classical Cepheid

Details Shock phenomena in a hydrodynamic model of a classical Cepheid Shock phenomena in a hydrodynamic model of a classical Cepheid

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pasj...43..795i&link_type=abstract

Astronomical Society of Japan, Publications (ISSN 0004-6264), vol. 43, no. 6, 1991, p. 795-807.

Astronomy and Astrophysics

Astronomy

4

Astronomical Models, Cepheid Variables, Hydrodynamics, Shock Waves, Stellar Oscillations, Stellar Luminosity, Stellar Mass, Stellar Temperature

Scientific paper

A hydrodynamic model of a classical Cepheid containing 500 grid points is compared with that containing 100 grid points. In linear models, the growth rates of the pulsation modes appear to grow as the number of grid points increases, and to saturate at about 200 meshes. In hydrodynamic models, some shock phenomena appear to be captured only in a 500-grid model. This indicates that a fine-grid model is very useful for studying the shock waves in a pulsating envelope. A newly constructed 500-grid model is applied to a study of the ionization/recombination fronts and shock waves in pulsating envelopes. The motion of discontinuities over an entire pulsation cycle is shown for the first time. At the minimum radius phase it is found that (1) the shock wave in the ionized region generates much heat energy, and that (2) the radiative flux significantly increases at the shock wave in the atmosphere. The above two results indicate that the inclusion of convective energy transport and/or that of improved radiative transfer may affect the behavior of a hydrodynamic model with a strong shock.

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