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High-frequency modes in solar-like stars

High-frequency modes in solar-like stars

Publication date: 01 November 2007

Authors: Karoff, C.

Journal: Monthly Notices of the Royal Astronomical Society
Volume: 381
Issue: 3
Page: 1001-1008
Year: 2007

Copyright: Blackwell Publishing

p-mode oscillations in solar-like stars are excited by the outer convection zone in these stars and reflected close to the surface. The p modes are trapped inside an acoustic cavity, but the modes only stay trapped up to a given frequency [known as the acoustic cut-off frequency (vac)] as modes with larger frequencies are generally not reflected at the surface. This means that modes with frequency larger than the acoustic cut-off frequency must be travelling waves. The high-frequency modes may provide information about the physics in the outer layers of the stars and the excitation source and are therefore highly interesting as it is the estimation of these two phenomena that cause some of the largest uncertainties when calculating stellar oscillations. High-frequency modes have been detected in the Sun, in beta-Hydri and in alpha-Cen A and alpha-Cen B by smoothing the so-called echelle diagram and the large frequency separation as a function of frequency has been estimated. The large frequency separation has been compared with a simple model of the acoustic cavity which suggests that the reflectivity of the photosphere is larger at high frequency than predicted by standard models of the solar atmosphere and that the depth of the excitation source is larger than what has been estimated by other models and might depend on the order n and degree l of the modes.

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