Current convection in solar active regions

Details Current convection in solar active regions Current convection in solar active regions

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993soph..145..111m&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 145, no. 1, p. 111-118.

Physics

4

Convection, Electric Current, Solar Corona, Solar Magnetic Field, Sunspots, Plasma Conductivity, Turbulent Diffusion, Vorticity

Scientific paper

The linear growth rates and wavelengths of unstable convective modes caused by the large gradient of electrical conductivity are found. The unstable modes produce fine-scale vortices perpendicular to the magnetic field, which overshoot well into the solar corona. The modes provide a turbulent vorticity source at the photospheric footpoints of the field. This can cause braiding and reconnection of the coronal magnetic field. The modes twist the coronal magnetic field into loops with a typical radius of 200 km, consistent with recent X-ray observations.

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