Hydrodynamic models for population-II cepheids |
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| Authors: | Yu A Fadeyev A B Fokin |
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| Institution: | (1) Astronomical Council of the USSR Academy of Sciences, Moscow, Germany |
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| Abstract: | The nonlinear self-excited pulsations of population-II stars with mass 0.6M
 and luminosities from 128 to 1280L
are studied. The pulsation periods are found to be in the range of 1.3 to 19 days. An increase of the stellar luminosity is shown to be accompanied by an increasing nonadiabaticity and decreasing efficiency of the radiative damping region. This leads to both an increase of the growth rate while pulsations are exciting and an increase of the oscillation amplitude of the limit cycle. In the models withL 800L
the efficiency of the radiative damping region becomes so small that amplitude growth ceases due to a dissipation of the mechanical energy by shocks in the stellar atmosphere. The models with periods of from 1.3 to 3 days show the bump on their light curves. The bump is connected with a travelling pulse generated at the antinode of the second overtone at maximum compression. The time delays estimated for the pulses reflected of the stellar core are in a good agreement with the pulse resonance condition proposed by Aikawa and Whitney (1983). The model with the period of 2.1 days revealed double resonance  0 = 22, 20 = 31 causing alternating oscillations with slightly different periods and amplitudes. The models with period of 10 days and longer reveal the resonance 0 = 21. This resonance causes the flat top on the light curve at a period of about 10 days and appearance of a shallow alternating minimum at longer periods, as is observed in RV Tau variables. The theoretical period-luminosity relation proposed for population-II cepheids is in good agreement with that obtained from observations. |
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