Solar differential rotation due to magnetic stresses

Details Solar differential rotation due to magnetic stresses Solar differential rotation due to magnetic stresses

Jun 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...259..663v&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 259, no. 2, p. 663-668.

Astronomy and Astrophysics

Astronomy

3

Magnetic Field Configurations, Planetary Waves, Solar Activity Effects, Solar Convection (Astronomy), Solar Magnetic Field, Solar Rotation, Helioseismology, Solar Interior, Sunspots

Scientific paper

It is argued that the components of differential rotation of the convection zone (defined as the deviation from rigid rotation) may be driven by Maxwell stresses. The zonally averaged flow within the upper convection zone is described by Rossby-Haurwitz waves of zonal wavenumber m = 0, and an estimate is given of the configuration of the poloidal and the toroidal magnetic fields necessary to drive the observed differential rotation. The magnetic field components derived for minimum and maximum solar activity are not inconsistent with the solar magnetic fields measured at the solar surface.

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