Global Magnetic Reversal in a Rapidly Rotating Sun

Details Global Magnetic Reversal in a Rapidly Rotating Sun Global Magnetic Reversal in a Rapidly Rotating Sun

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.0804n&link_type=abstract

American Astronomical Society, SPD meeting #40, #8.04; Bulletin of the American Astronomical Society, Vol. 41, p.816

Astronomy and Astrophysics

Astronomy

Scientific paper

Global MHD simulations of the solar convection zone and a tachocline of shear at its base have demonstrated that strong bands of toroidal magnetic field can be built in the tachocline through stretching and organizing of small-scale fields that have been pumped downward into it. Recent 3-D simulations of more rapidly rotating suns have revealed that global-scale wreathes of toroidal magnetic field can even be achieved in the bulk of the convection zone itself, remarkably without a tachocline of shear present at its base. Continuing this work, we simulate a sun without a tachocline, rotating at three times the solar rate, and at a higher turbulence level than previous simulations. We find toroidal magnetic wreathes which have large temporal variations in field strength as they interact with turbulent convection and global differential rotation, yet rebuild themselves, persisting in the bulk of the convection zone for thousands of days. These magnetic structures can even undergo a reversal of global magnetic polarity, and may persist in this state for some time. We describe here the nature of such a reversal and the relative timing of changes in the poloidal and toroidal fields.

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