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Astron. Astrophys. 337, L29-L33 (1998)

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2. Input physics and numerical method

For the nonlinear modelling of stellar pulsations we solve the full system of radiation hydrodynamics (RHD) together with a time-dependent model of turbulent convection developed by Kuhfuss (1986) and reformulated for coupling with the RHD-system by Wuchterl (1995). Time-dependent radiative transfer is included in the grey approximation, opacities are taken from the OPAL project (Iglesias & Rodgers 1991) and below 6000 K we use the molecular opacities provided by Alexander et al. (1989). The equation of state has been taken from Wuchterl (1990). All nonlinear limit cycle computations are started from hydrostatic envelope models and the pulsation is initiated through an appropriate initial velocity perturbation (Stobie 1969). The numerical solution is based on the adaptive grid equation developed by Dorfi & Drury (1987) which distributes the spatial grid points according to accuracy considerations. For further details we refer to Dorfi & Feuchtinger (1995), Feuchtinger & Dorfi (1998) and to a forthcoming paper.

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© European Southern Observatory (ESO) 1998

Online publication: August 17, 1998
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