Convection zone origins of solar atmospheric heating

Details Convection zone origins of solar atmospheric heating Convection zone origins of solar atmospheric heating

Oct 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...309..864s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 309, Oct. 15, 1986, p. 864-873.

Astronomy and Astrophysics

Astrophysics

3

Convection Currents, Coronas, Solar Atmosphere, Solar Heating, Spicules, Atmospheric Circulation, Flow Equations, Magnetohydrodynamic Waves, Solar Energy, Solar Magnetic Field

Scientific paper

Spicules are examined as a means for supplying the corona with mass, energy, and magnetic field. It is suggested that spicules form from the supersonic upward expansion of material on nearly evacuated network flux tubes embedded within the sun's convection zone. This allows supersonic but subescape velocities to be attained by the material as it flows outward through the photosphere. Although supersonic, the kinetic energy (subescape) of the spicule material, as observed, is insufficient for coronal heating. It is suggested that, through buoyancy changes on evacuated flux tubes, the magnetic field first 'wicks' material flow into the solar atmosphere. Subsequently, the magnetic field energizes the gaseous material to form the conventional hot, dynamically expanding, solar corona. This occurs through momentum and energy transport by Alfven waves and associated Maxwell stresses concurrently flowing upward on these 'geysers' (spicules). The vertical momentum equation governing fluid flow is examined, and a particular equipartition solution is presented for the flow velocity along a simple field geometry.

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