The Contribution of Sound Waves and Instabilities to the Penetration of the Solar Differential Rotation Below the Convection Zone

Details The Contribution of Sound Waves and Instabilities to the Penetration of the Solar Differential Rotation Below the Convection Zone The Contribution of Sound Waves and Instabilities to the Penetration of the Solar Differential Rotation Below the Convection Zone

Feb 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004soph..219..231d&link_type=abstract

Solar Physics, v. 219, Issue 2, p. 231-250 (2004).

Physics

Scientific paper

The response of a layer to a horizontal shear flow at its top the surface was studied numerically as an initial value problem. The geometry was Cartesian and the conservation equations were solved with the help of the Zeus-3D code. In the initial state, the pressure, p, and density, ρ, of the layer were assumed to be related by a polytropic equation of index 1.14, which best approximates the solar values in the region of interest. The values of p and ρ at the lower boundary of the layer, namely r=R l=0.4 R &sun;, were taken to be the solar values. The upper boundary was chosen to be the base of the solar convection zone, r=R c=0.7 R &sun;. The shear flow at the surface, v φ(R c), was proportional to the solar differential rotation, and acoustical oscillations were present in the layer.

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