Meridional Drift of Large-Scale Solar Magnetic Fields

Details Meridional Drift of Large-Scale Solar Magnetic Fields Meridional Drift of Large-Scale Solar Magnetic Fields

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003arep...47..333o&link_type=abstract

Astronomy Reports, vol. 47, Issue 4, p.333-342

Astronomy and Astrophysics

Astronomy

5

Scientific paper

It is shown that the meridional drift of large-scale fields starts in the equatorial zone and continues over 15 16 yrs (16 17 according to another estimate), i.e., during three fourths of the 22-year cycle. There is an abrupt retardation of the drift at latitudes of 30° 50°, and a stagnation region where the drift rate does not exceed several meters per second arises. The drift becomes rapid again at higher latitudes. The stagnation region coincides with the area in which the radial gradient of the rotational velocity is close to zero in the convective zone. This drift is compared with helio-seismological data on the rotation in the convective zone. A model taking into account some elements of dynamo theory is proposed.

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