Physics
Scientific paper
Jan 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001esasp.464..535m&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,
Physics
3
Convection Zone, Convective Overshoot, Latitude, Tachocline, Solar Cycle
Scientific paper
A we approach the solar maximum for the current cycle it is timely to establish what helioseismology can tell us about the internal changes the Sun undergoes as the cycle progresses. In this work we use SOI-MDI data in order to identify changes occurring to the stratification of the Sun at the base of the convective envelope. Both changes with time (averaged over colatitude) and changes over time at different colatitudes are addressed. These are discussed in terms of the changes in the properties of the convection at the base of the envelope in the region where the tachocline is present. Those variations could be attributed to the interaction between convection, rotation and magnetic fields, which must be intrinsically time-dependent phenomena, possibly correlated with the observed changes occurring over the cycle in the envelope up to the surface.
Christensen-Dalsgaard Joergen
Monteiro Mario J. P. F. G.
Schou Jepser
Thompson Michael J.
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