Other
Scientific paper
Aug 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983natur.304..520s&link_type=abstract
Nature (ISSN 0028-0836), vol. 304, Aug. 11, 1983, p. 520-522. Sponsorship: Science and Engineering Research Council.
Other
19
Angular Momentum, Solar Interior, Solar Rotation, Angular Velocity, Baroclinic Instability, Magnetohydrodynamic Stability, Solar Oscillations, Stellar Interiors
Scientific paper
It is noted that the low surface rotation rate of the sun and other mainsequence stars is believed to be the result of angular momentum loss due to a stellar wind. This loss also gives rise to a differential rotation, the interior spinning more rapidly than the surface. The rate of increase with depth of the rotation speed is limited by hydrodynamic instabilities, which result in an outward diffusion of angular momentum. The conditions for the occurrence of hydrodynamic instabilities in a radiative stellar interior are reviewed here on the assumption that the rotation is constant on spheres. The instability with the lowest threshold is double diffusive, referred to as the axisymmetric baroclinic diffusive instability. A minimum rotation curve for the present sun is calculated on the assumption that the efficiency of this instability is sufficiently high that the rotation of the sun is close to marginal stability. This lower limit to the internal rotation rate is roughly consistent with current observations of the rotational splitting of solar oscillations.
Knobloch Eberhard
Roxburgh Ian W.
Spruit Hendrik C.
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