Non-adiabatic oscillations of the low- and intermediate-degree modes of the Sun

Details Non-adiabatic oscillations of the low- and intermediate-degree modes of the Sun Non-adiabatic oscillations of the low- and intermediate-degree modes of the Sun

Jul 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010mnras.405.2759x&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 405, Issue 4, pp. 2759-2767.

Astronomy and Astrophysics

Astronomy

1

Convection, Sun: Oscillations

Scientific paper

Using a non-local time-dependent theory of convection, the linear stability is analysed for low- and intermediate-degree (l = 1-25) g4-p39 modes of the Sun. The results show that all the p modes with periods from ~3 to ~16min are pulsationally unstable, while all the g, f and p modes with periods longer than ~16min and the high-frequency p modes with periods shorter than ~3min are stable except the low-degree (l = 1-5) p1 modes. The pulsation amplitude growth rates depend on only the frequency and almost do not depend on l. They achieve the maximum at ν ~ 3700μHz (P ~ 270s). The effects of radiation and convection on the stability are analysed in detail. The coupling between convection and oscillations plays a key role for stabilization of low-frequency f and p modes and excitation of intermediate- and high-frequency p modes. We propose that the solar 5-min oscillations are not excited by a single mechanism, but are resulted from the combined effects of the `regular' coupling between convection and oscillations and the turbulent stochastic excitation. The coupling between convection and oscillations is the dominant excitation and damping mechanism for the low- and intermediate-frequency modes, and the turbulent stochastic excitation is the main excitation mechanism for high-frequency p modes.

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