2011/07/07 by Dennis Stello, D. Stello, Stello, D. · 1 citation
Physics and Astronomy · #Astronomy and Astrophysical Research #FOS: Physical sciences #Scientific Research and Discoveries #Solar and Stellar Astrophysics (astro-ph.SR) #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.48550/arxiv.1107.1311
11 pages, 7 figures, To appear in the ASP proceedings of "The 61st Fujihara seminar: Progress in solar/stellar physics with helio- and asteroseismology", 13th-17th March 2011, Hakone, Japan. Ed: Hiromoto Shibahashi
openalex publication_date 2011/07/07 · arxiv created 2011/07/18 · arxiv updated 2011/07/20 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
In cool stars that oscillate like the Sun, non-radial modes become mixed as the stars evolve. The mixing is caused by the coupling between g-modes in the stellar core and p-modes in the envelope, which results in distinctly different and more complex frequency spectra for subgiants and red giants than seen in main sequence stars. Using a new version of the `scaled' échelle diagram, I illustrate how the frequencies of non-radial modes evolve during the evolution from the main sequence to the red giant branch, and I show how they depend on stellar mass and metallicity. Then, with focus on the dipole (l = 1) modes, which show the strongest effects from mixing, I present a toy model to fit, and hence identify, those modes in a large series red giant models.