Double-mode stellar pulsation

Details Double-mode stellar pulsation Double-mode stellar pulsation

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993ap%26ss.210..281k&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 210, no. 1-2, p. 281-300 (IAU Colloquium 134)

Astronomy and Astrophysics

Astrophysics

2

Convective Flow, Hydrodynamics, Stellar Models, Stellar Oscillations, Variable Stars, Lyra Constellation, Numerical Stability, Turbulent Flow

Scientific paper

The current observational and theoretical status of the double-mode variables is reviewed. Focusing mostly on the RR Lyrae stars, we address the question of the observational evidence of modal stability. The problem of stationarity is a crucial issue in the modeling of these stars. We mention past efforts in hydrodynamical and analytical modeling together with a detailed discussion of some very recent results. It is suggested that stochastic forcing due to turbulent convection may play a crucial role in exciting some marginally stable modes in the limiting pulsation. The latest hydrodynamical results first demonstrate that purely radiative models are able to show permanent double-mode behavior in the relevant period regime of RRd stars. The reason for the previous lack of double-mode behavior is attributed to the large dissipation, i.e. artificial viscosity, generally used in the codes to ensure numerical stability and to obtain amplitudes comparable to the observed ones. We think that better models should include some physical dissipation, most probably turbulent convection, and a more accurate numerical treatment of the radiative hydrodynamics.

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