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Dynamical Processes Induced by the Internal Solar Rotation

Published online by Cambridge University Press:  26 May 2016

S. Turck-Chièze
S. Turck-Chièze*
Affiliation:
CEA/DAPNIA/SAp, CE Saclay, 91191 Gif sur Yvette Cedex, FRANCE

Abstract

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Helioseismology has been developed to extract internal sound speed, rotation and magnetic field. Such informations will put strong constraints on the present missing dynamical phenomena. Starting from the present observations on the rotation, I discuss quantitatively two important regions, the transition region between radiation and convection, called tachocline and the radiative region. In the tachocline, lithium indicator shows that a turbulent mixing is certainly present in main sequence solar like stars. on the other end, a detailed study of pre-main sequence stars encourages also the introduction of magnetic effects in addition to such a term below 10 Myr. For the solar radiative zone, the difficulty to determine the rotation profile is first noticed and discussed showing the great advantage of the gravity modes or mixed modes in addition to the acoustic modes. A possible profile, decreasing from 0.4 to 0.2 R⊙ and then increasing in the very central region is suggested by the present observations. The consequences in terms of dynamical processes are discussed.

Type
Session 3 Rotation, Solar and Stellar Physics
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 317 - 322
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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