Influence of the perturbation of the Reynold tensor on the stability of the solar 5-minute oscillations

Details Influence of the perturbation of the Reynold tensor on the stability of the solar 5-minute oscillations Influence of the perturbation of the Reynold tensor on the stability of the solar 5-minute oscillations

Mar 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...175..125g&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 175, no. 1-2, March 1987, p. 125-135.

Astronomy and Astrophysics

Astrophysics

9

Perturbation Theory, Solar Oscillations, Stable Oscillations, Stress Tensors, Convective Heat Transfer, Magnetohydrodynamic Stability, Radiative Transfer, Viscous Flow

Scientific paper

It is believed that the 5 min solar oscillations are linearly stable and that they are excited by nonlinear coupling with convection. However two terms of the coefficient of vibrational stability have been ignored so far. They are both connected to the perturbation of the Reynold tensor. The author has computed these two terms for isotropic and non isotropic convection using the theory of interaction between convection and pulsation of Gabriel et al. (1974). The influence of these 2 terms on the stability of 5 min oscillations of low, intermediate and high degree l is calculated. For low and intermediate l all the modes considered are found unstable while for high l only modes of order or lower than a value n*, decreasing as l increases, are unstable. Comparison with observations suggests a good agreement. For all l the most unstable mode has a period between 5 and 6 min and have an e-folding time which decreases from 0.22 yr to 0.014 yr as l increases from 2 to 600.

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