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Astron. Astrophys. 329, 315-318 (1998)

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Towards a hydrodynamical model
predicting the observed solar rotation profile

Suzanne Talon and Jean-Paul Zahn

Département d'Astrophysique Stellaire et Galactique, Observatoire de Paris, Section de Meudon, F-92195 Meudon, France (Suzanne.Talon@obspm.fr, Jean-Paul.Zahn@obspm.fr)

Received 24 June 1997 / Accepted 19 August 1997


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.

Key words: hydrodynamics – turbulence – Sun: interior – Sun: rotation – stars: interiors – stars: rotation

Send offprint requests to: Suzanne Talon

© European Southern Observatory (ESO) 1998

Online publication: November 24, 1997