Physics
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992soph..139...47c&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 139, no. 1, May 1992, p. 47-64.
Physics
25
Solar Corona, Solar Magnetic Field, Solar Prominences, Ultraviolet Emission, Extreme Ultraviolet Radiation, Magnetohydrodynamic Waves, Solar Radiation, Solar Temperature, Stellar Models
Scientific paper
A model is developed to analyze the emissions from the prominence-corona transition region (PCTR), and comparisons are made with observational data to assess the heating mechanism in the PCTR. The cool matter of the quiescent filaments is assumed to be organized into magnetic flux loops in the hot coronal cavity gas. The lower layers of the PCTR are theorized to be heated by the dissipation of Alfven waves since the heating caused by the divergence of transverse conduction is not consistent with EUV and UV emissions. The temperature gradient of the high-temperature layers is determined by the balance of radiative cooling and conductive heating with magnetic fields minimizing thermal conduction. The model offers an explanation for the difference in observed EUV brightnesses at the limb and on the disk caused by the angle between the filaments and the line of sight.
Chuideri Drago Franca
Engvold Oddbjörn
Jensen Eberhart
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