Semiclassical approximation for low-degree stellar p modes - II. Classical ray tracing

Details Semiclassical approximation for low-degree stellar p modes - II. Classical ray tracing Semiclassical approximation for low-degree stellar p modes - II. Classical ray tracing

Sep 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000mnras.317..151r&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 317, Issue 1, pp. 151-157.

Astronomy and Astrophysics

Astronomy

13

Waves, Methods: Numerical, Stars: Oscillations

Scientific paper

Using ray-tracing techniques, we consider nearly forward refraction in the stellar interior of acoustic waves modified by buoyancy and gravity. Our analysis is based on a local dispersion relation developed to second order in the high-frequency asymptotic approximation. The phase shifts δlδ0(ω)+l(l+1)Dδ (ω) of the partial waves of stellar p modes, which govern the eigenfrequency equation in its classical limit, are developed in terms of explicit integrals containing the radial profiles of seismic parameters in the stellar interior. The accuracy of the resulting description of low-degree stellar p modes is tested using an evolutionary sequence of solar models.

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