Physics
Scientific paper
May 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994soph..151..265l&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 151, no. 2, p. 265-270
Physics
22
Convective Flow, Magnetic Field Reconnection, Solar Prominences, Solar Temperature, Spectroscopic Analysis, Atmospheric Models, Chromosphere, Convection Currents, Coronal Loops, Magnetic Disturbances, Photosphere
Scientific paper
Magnetic reconnection at the photospheric boundary is an essential part of some theories for prominence formation. We consider a simple model for reconnection in this region. Parameters of the reconnecting current sheet are expressed in terms of the concentration and temperature of the outside dense and cold plasma, magnetic field intensity, and velocity of convective flows at the photosphere. The reconnection process is shown to be most efficient in a layer several hundred kilometers thick coinciding with the temperature minimum region of the solar atmosphere. The calculated upward flux of matter through the current sheet (approximately equals 1011-1012 g/s) is amply sufficient for prominence formation in the upper chromosphere or lower corona.
Litvinenko Yu. E.
Somov Boris V.
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