The nature of the sunspot phenomenon. III - Energy consumption and energy transport. IV - The intrinsic instability of the magnetic configuration

Details The nature of the sunspot phenomenon. III - Energy consumption and energy transport. IV - The intrinsic instability of the magnetic configuration The nature of the sunspot phenomenon. III - Energy consumption and energy transport. IV - The intrinsic instability of the magnetic configuration

Feb 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975soph...40..275p&link_type=abstract

Solar Physics, vol. 40, Feb. 1975, p. 275-289, 291-301.

Physics

16

Convective Flow, Energy Transfer, Solar Energy, Solar Magnetic Field, Sunspots, Energy Conversion, Magnetic Field Configurations, Magnetohydrodynamic Stability, Solar Atmosphere, Thermal Energy

Scientific paper

The basic relation is described between conversion of thermal energy into convective fluid motion and convective transport of thermal energy, and the equilibrium configuration of a sunspot's magnetic field is shown to be unstable to the hydromagnetic exchange instability. It is determined that heat transport necessarily accompanies convective driving of fluid motion and that the formation of cool sunspots requires convection extending coherently over several scale heights, a distance of at least 500 km. Several theoretical possibilities for sunspot stabilization are reviewed, and it is suggested that a suitable redistribution of cooling in the umbra may be the stabilization mechanism. It is believed that if cooling extends to a great depth in an elongated portion of a sunspot, the magnetic pressure on the boundary will be reduced, tending to reduce the elongation.

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