Towards a hydrodynamical model predicting the observed solar rotation profile

Details Towards a hydrodynamical model predicting the observed solar rotation profile Towards a hydrodynamical model predicting the observed solar rotation profile

Jan 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...329..315t&link_type=abstract

Astronomy and Astrophysics, v.329, p.315-318 (1998)

Astronomy and Astrophysics

Astrophysics

23

Hydrodynamics, Turbulence, Sun: Interior, Sun: Rotation, Stars: Interiors, Stars: Rotation

Scientific paper

We present here the results of a numerical study performed to investigate the role of gravity waves in the evolution of the solar rotation profile. We show that, together with meridional circulation and shear turbulence, they may enforce solid body rotation in the solar interior. The transient phase is characterized by an outer portion of the radiative zone rotating at the velocity of the convection zone and an inner portion in strong differential rotation with depth. The gravity waves slow down the outer portion, whereas it is the meridional circulation which dominates the transport of momentum in the interior. With our treatment of the excitation and damping of these waves, solid body rotation is achieved on a timescale of a few giga-years, depending on the initial velocity of the model.

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