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
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DOI：
10.1111/j.1365-2966.2010.16662.x
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发表时间：
2010-07-11
影响因子：
4.8
通讯作者：
Deng, L.
中科院分区：
文献类型：
--
作者：
Xiong, D. R.;Deng, L.
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 similar to 3 to similar to 16 min are pulsationally unstable, while all the g, f and p modes with periods longer than similar to 16 min and the high-frequency p modes with periods shorter than similar to 3 min 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 nu similar to 3700 mu Hz (P similar to 270 s). 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.
