Critical layers for internal waves in stellar radiation zones

Details Critical layers for internal waves in stellar radiation zones Critical layers for internal waves in stellar radiation zones

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011sf2a.conf..443a&link_type=abstract

SF2A-2011: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics Eds.: G. Alecian, K. Belkacem,

Astronomy and Astrophysics

Astrophysics

Internal Gravity Waves, Critical Layers, Angular Momentum Transport

Scientific paper

Internal waves are candidates for explaining stellar radiation zone angular velocity profiles, for example in the Sun. The equation describing the adiabatic and inviscid propagation of such waves is singular at a `` critical level'' where the fluid rotation frequency is proportional to the wave frequency. Here, we propose a generalization of previous studies to the stellar, spherical case. We resolve the problem by three methods, depending on the value of the Richardson number at the critical level Ri_c and our results can be divided into two cases. If (l(l+1)/m^2) Ri_c is larger than 1/4, waves are attenuated by a factor depending on Ri_c as they pass through a critical level. If (l(l+1)/m^2) Ri_c is less than 1/4, the basic flow is then unstable and the wave can be reflected with a coefficient larger than 1. In the latter case, the process is called over-reflection.

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