Some MHD Solutions for the Bottom of the Solar Convective Layer

Details Some MHD Solutions for the Bottom of the Solar Convective Layer Some MHD Solutions for the Bottom of the Solar Convective Layer

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aspc..370...74c&link_type=abstract

Solar and Stellar Physics Through Eclipses ASP Conference Series, Vol. 370, proceedings of the conference held 27-29 March, 2006

Physics

Scientific paper

The magnetic field responsible for the solar activity is stored in the base of the convective zone. Applying this knowledge to the bottom of the convection zone in the Sun our objective was to investigate some magnetohydrodynamical (MHD) solutions. The first order perturbation approximation was used in order to calculate the small perturbations on the physical parameters of a Standard Solar Model (SSM) excluding both rotation and magnetic field (Christensen-Dalsgaard et al. 1996) in the unperturbed equilibrium case. The validity of each approximation is tested and examined from the SSM. The MHD results thus obtained are presented graphically and compared with those of the SSM.

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