2007/05/02 by G. J. Savonije · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #Computational astrophysics #Eigenfunction #Harmonic #Rotation (mathematics) #Scientific Research and Discoveries #Spherical harmonics #Star (game theory) #Stars #Stellar pulsation #Stellar rotation #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1051/0004-6361:20077377
7 pages, 7 figures; accepted by A&A
openalex publication_date 2007/05/02 · arxiv created 2007/05/12 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Context.Oscillations in rotating stars with frequency of the same order or smaller than the rotation rate Ω cannot be described by a single spherical harmonic due to the effect of the Coriolis force. This is a serious complication which is usually treated by writing the eigenfunctions as a (truncated) sum of different spherical harmonic degrees for a given m-value, or by neglecting the θ part of the rotation vector (Traditional Approximation).