Structure of the solar tachocline: confrontation of theoretical models with SOHO/MDI helioseismic constraints

Details Structure of the solar tachocline: confrontation of theoretical models with SOHO/MDI helioseismic constraints Structure of the solar tachocline: confrontation of theoretical models with SOHO/MDI helioseismic constraints

Jun 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004padeu..14..177f&link_type=abstract

In: Proceedings of the British-Hungarian N+N Workshop for Young Researchers On Computer processing and use of satellite data in

Astronomy and Astrophysics

Astrophysics

Scientific paper

Helioseismic measurements indicate that the solar tachocline is very thin, its full thickness not exceeding 4% of the solar radius. The mechanism that inhibits differential rotation to propagate from the convective zone to deeper into the radiative zone is not known, though several propositions have been made. We present detailed numerical calculations of the fast solar tachocline based on the assumption that the dynamo field dominates over the dynamics of the tachocline.

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