Solar prominence magnetic configurations derived numerically from convection

Details Solar prominence magnetic configurations derived numerically from convection Solar prominence magnetic configurations derived numerically from convection

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26a...371..328m&link_type=abstract

Astronomy and Astrophysics, v.371, p.328-332 (2001)

Astronomy and Astrophysics

Astrophysics

Supergranulation, Convection, Prominences

Scientific paper

The solar convection zone may be a mechanism for generating the magnetic fields in the corona that create and thermally insulate quiescent prominences. This connection is examined here by numerically solving a diffusion equation with convection (below the photosphere) matched to Laplace's equation (modeling the current free corona above the photosphere). The types of fields formed resemble both Kippenhahn-Schlüter and Kuperus-Raadu configurations with feet that drop into supergranule boundaries.

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