Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993ap%26ss.210..231g&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 210, no. 1-2, p. 231-233 (IAU Colloquium 134)
Astronomy and Astrophysics
Astrophysics
Stellar Mass, Stellar Models, Stellar Oscillations, Stellar Structure, Variable Stars, Amplitudes, Astronomical Photometry, Hydrodynamics, Nonlinearity
Scientific paper
Efficient tools of investigation of stellar pulsation are the integral relations which link oscillation frequencies to the static structure of stellar models, as provided by the linear theory of pulsation. Similarly, oscillation amplitudes and phases, which arise from nonlinear processes, can be related to the stellar structure by means of amplitude equation formalisms. For the simple case of a monoperiodic oscillation, involving only one unstable marginal mode, such a formalism shows that the (limit cycle) radius variations, at time t and mass level m, can be approximated, up to second order of approximation. The nonlinear, nonadiabatic coefficients, are integrals over mass of kernels which depend on eigenfrequencies, eigenfunctions, on second and third order Taylor quantities from the equations modelling the star. They can either be computed from static models (Klapp et al., 1985) or obtained by numerical fits of hydrodynamical results (Kovacs and Buchler, 1989).
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