Turbulent convection and pulsational stability of variable stars: non-adiabatic oscillations of the solar p-modes

Details Turbulent convection and pulsational stability of variable stars: non-adiabatic oscillations of the solar p-modes Turbulent convection and pulsational stability of variable stars: non-adiabatic oscillations of the solar p-modes

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000mnras.319.1079x&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 319, Issue 4, pp. 1079-1093.

Astronomy and Astrophysics

Astronomy

13

Convection, Sun: Oscillations

Scientific paper

By using a non-local time-dependent theory of convection, the non-adiabatic oscillations of the radial p-modes of the Sun were calculated. The coupling between convection and oscillation and the influence of departure from radiative equilibrium on oscillations of p-modes were investigated in detail. The results of numerical calculations show that when the coupling between convection and oscillations is ignored, all the low-order radial p-modes with n<~10 are pulsationally unstable and all the intermediate- and high-order (n>~11) radial p-modes are pulsationally stable. When the coupling between convection and oscillations is taken into consideration, only the intermediate-order p-modes with 11<~n<~23 are pulsationally unstable and all the low-order (n<~10) and high-order (n>~24) p-modes are pulsationally stable. The behaviour of stability of the solar p-mode oscillations described above is the result of the joint action of radiation and convection on oscillations. In the interior of the convection zone, the thermodynamic coupling between convection and oscillations gives rise to damping of solar oscillations, but at the top of the convection zone, it causes excitation. The thermodynamic coupling between convection and oscillations plays a key role in the stabilization of low-frequency solar p-modes and also in the excitation of the intermediate-order solar p-mode oscillations with periods of about 5min. The turbulent pressure generally causes excitation. The radiative damping in the outer atmosphere and the turbulent viscosity are the main damping mechanisms of the high-order (ν>~4000μHz) solar p-modes. For the low-order p-mode oscillations with ν<~1000μHz, the departure from radiative equilibrium (DRE) does not have a significant effect. With the increase of frequency, the influence of the outer atmosphere and the DRE grows rapidly. The generalized Eddington approximations (GEA) developed by Unno & Spiegel and Mihalas are much better than the usual radiative diffusion approximation. Our conclusion is as follows: the coupling between convection and oscillations is an important excitation and damping mechanism for solar 5-min oscillations. However, it cannot be used to interpret all the observational characteristics of solar p-modes. There must be excitation and damping mechanisms other than the radiation and the `regular' coupling between convection and oscillations.

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