The Magnetic Field in the Convection Zone

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One of the key questions in solar physics that remains to be answered concerns the strength and the distribution of the magnetic fields at the base of the convection zone. The flux tube dynamics requires that toroidal fields of strength as large as 100 kilogauss be present at the base of the convection zone. The kinetic-magnetic equipartition argument leads to smaller field strengths. For possible detection of these relatively small (compared to pressure effects) fields by helioseismic methods it is important to know the range of the field strengths and their distribution. We estimate a range for the toroidal magnetic field strengths at the base of the convection zone using dynamo simulations in a spherical shell. These simulations involve the distribution of rotation provided by helioseismic inversions of the GONG and MDI data. Combining the simulations with the observed line-of-sight surface poloidal field we extract the spatial pattern and magnitude of the mean toroidal magnetic field at the base of the convection zone.
To be published in the proceedings of "SOHO 12 / GONG+ 2002 Local and Global Helioseismology: The Present and Future" October 27 to November 1, 2002 Big Bear Lake, California

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http://salesiana.dossiersoluciones.com/handle/123456789/5297

Consulte el texto completo en el siguiente enlace:

https://arxiv.org/abs/astro-ph/0211116
 http://arxiv.org/abs/astro-ph/0211116
 Proc. of SOHO 12/GONG+ 2002 'Local and Global Helioseismology: The Present and Future', Big Bear Lake, California (U.S.A.), 27 October - 1 November 2002 (ESA SP-517, February 2003) ISSN 0379-6566 / ISBN 92-9092-827-1

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arXiv