Open AccessSemiclassical approximation for low‐degree stellar p modes – II. Classical ray tracing
Author(s) -
Roxburgh I. W.,
Vorontsov S. V.
Publication year - 2000
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2000.03624.x
Subject(s) - physics , ray tracing (physics) , dispersion relation , semiclassical physics , astrophysics , limit (mathematics) , buoyancy , velocity dispersion , classical mechanics , mathematical analysis , optics , quantum mechanics , galaxy , mathematics , quantum
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 δ ℓ δ 0 ( ω )+ℓ(ℓ+1) D ( 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.