Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984ap%26ss.100..329f&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 100, no. 1-2, March 1984, p. 329-339.
Astronomy and Astrophysics
Astrophysics
25
Stellar Luminosity, Stellar Models, Stellar Oscillations, Variable Stars, Hydrodynamic Equations, Kinetic Energy, Light Curve, Nonlinear Systems, Stellar Mass
Scientific paper
The radial nonlinear pulsations of a model with M = 0.8 M_sun;, Mbol = -6 mag and Teff = 5500K have been studied. The pulsations are shown to exist in the form of the standing wave only in the innermost layers with R < 0.2 Rph. In the outer layers, the standing wave transforms into runnig waves, the frequency of which decreases with an increasing R. The pulsation period at the photosphere is found to be twice as long as the pulsation period at R < 0.2 Rph. The difference between the pulsation periods causes alternation of deep and shallow minima in the temporal dependences of the kinetic energy and radii and can be used to explain the nature of RV Tau variables. It is shown that at the distance R > 3 Rph, the time-independent mass flux caused by shocks takes place. The rate of mass loss is found to be M≡ 10-4 M_sun; yr-1.
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