Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007smma.conf..300f&link_type=abstract
Spectroscopic methods in modern astrophysics. Proceedings of the conference held 13-15 September 2006, Moscow, Russia. Eds. L. M
Astronomy and Astrophysics
Astrophysics
Scientific paper
Nonlinear modelling of pulsating stars has two main features. Firstly, a self-consistent time-dependent model must include not only the optically thin atmospheric region, but also the subphotospheric envelope, where the instability regions are located. The physical conditions and spatial scales of these regions are very different, while the accuracy of calculations should be as high as possible, especially for the radiative shock waves. As numerical experiments show, the loss of accuracy in the description of the atmospheric dynamics may seriously affect the calculated motions in the inner region, and vice versa, to say nothing of the synthetic line spectrum which is one of the main goals of the atmosphere modelling. Secondly, to obtain the attractor (normally -- the limit cycle) we must run the hydromodel for about 10^3 to 10^4 pulsational cycles, or even more, with thousands of intermediate models (i.e. time steps) per one cycle. It is thus clear that we have to simplify the problem of the radiative hydrodynamics of pulsating atmospheres in order to obtain reliable result in a reasonable CPU time. In the present talk we describe one of possible approaches which gives good results at least in a semi-quantitative way. Here we discuss only radially pulsating stars.
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