The solar tachocline: Where do we stand?

Details The solar tachocline: Where do we stand? The solar tachocline: Where do we stand?

Jan 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001esasp.464..273b&link_type=abstract

In: Proceedings of the SOHO 10/GONG 2000 Workshop: Helio- and asteroseismology at the dawn of the millennium, 2-6 October 2000,

Computer Science

Sound

1

Sun, Tachocline

Scientific paper

This paper reviews some of the basic features of the tachocline of shear present at the base of the solar convective zone. We discuss some aspects of its dynamics and evaluate processes capable of stopping the spread of the shear deeper into the radiative interior. By taking into account the macroscopic mixing occuring within this thin layer, we can improve substantially the agreement between recent 1-D solar models and quantities inferred from observing the Sun, such as the radial sound speed profile or the photospheric abundances of light elements.

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