Hostname: page-component-7b7567c8c-jswmv Total loading time: 0 Render date: 2026-11-15T15:36:42.313Z Has data issue: false hasContentIssue false
  • English
  • Français

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

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the 'Save PDF' action button.

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.

Information

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 

References

Bouvier, J., Forestini, M, Allain, S., 1997, A & A 326, 1023 Google Scholar
Brun, A. S., Turck-Chieze, S., Zahn, J.P., 1999, ApJ 525, 1032 CrossRefGoogle Scholar
Brun, A. S. & Toomre, J., 2002, ApJ 570, 865 CrossRefGoogle Scholar
Corbard, T., et al., 1999, A & A 344, 696 Google Scholar
Chaboyer, B. & Zahn, J-P., 1992, A & A 253, 173 Google Scholar
Donahue, R. A., Saar, S. H., & Baliunas, S. L., 1996, ApJ 466, 384 CrossRefGoogle Scholar
Feigelson, E. D. et al., 2003, ApJ, in press astro-ph/0211049 Google Scholar
Fossat, E. & Salabert, D. et al., 2003, SoHO12-GONG2002, ESA Publication, p. 139 Google Scholar
Kosovichev, A. et al., 1997, Sol. Phys. 170, 43 CrossRefGoogle Scholar
Piau, L., 2001, Thesis University Paris VII Google Scholar
Piau, L., & Turck-Chieze, S., 2001, ApJ 566, 419 Google Scholar
Skumanich, A., 1972, ApJ 171, 565 CrossRefGoogle Scholar
Spiegel, E. A., & Zahn, J-P., 1992, A & A 265, 106 Google Scholar
Theado, S. & Vauclair, S., 2002, IAU colloquium 185, 70 Google Scholar
Turck-Chieze, S., et al., 2001a, Sol. Phys. 200, 323 CrossRefGoogle Scholar
Turck-Chieze, et al., 2001b, ApJ L555, L69 Google Scholar
Turck-Chieze, et al., 2001c, ESA-SP 464, 331 Google Scholar
Turck-Chieze, S. et al, 2002, ESA SP 508, 593 Google Scholar
Turck-Chieze, S. et al., 2003 ApJ submitted Google Scholar
Ventura, P., et al., 1998, A & A 331, 1011 Google Scholar
Watanabe, S & Shibahashi, H., 2001, PASJ 53, 565 CrossRefGoogle Scholar