Dynamics of coronal structures - Magnetic field-related heating and loop energy balance

Details Dynamics of coronal structures - Magnetic field-related heating and loop energy balance Dynamics of coronal structures - Magnetic field-related heating and loop energy balance

Jan 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...243..301g&link_type=abstract

Astrophysical Journal, Part 1, vol. 243, Jan. 1, 1981, p. 301-308. Research supported by the Smithsonian Institution and Consig

Astronomy and Astrophysics

Astrophysics

55

Coronal Loops, Magnetic Field Reconnection, Plasma Heating, Solar Corona, Solar Magnetic Field, Atmospheric Heating, Convection, Energy Budgets, Turbulent Flow

Scientific paper

The heating of the inhomogeneous solar corona is discussed in the context of local coronal magnetic field energy release and associated plasma heating. Expressions of general applicability relating the parameters characterizing heated and confined atmospheres to heating processes involving magnetic field reconnection are derived and then evaluated for a specific heating process. This work is thought to extend and refine previous models for the heating of confined coronal plasma structures. A theory for steady energy release is developed, and scaling laws are derived for the average coronal loop temperature and energy-release rate which are compared with similar (but parameter-free) scaling laws; this comparison makes it possible to determine the plasma beta and nonpotential magnetic field within coronal loop structures in the context of the model. Constraints on the applicability of static coronal loop atmosphere models are developed, and the close correlation between the thermal conductive loss and radiative loss for quasi-static confined loop atmospheres is shown.

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