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RADIATIVE COOLING OF STELLAR MATERIAL WITH APPLICATIONS TO SOLAR FLARES,
BOEING SCIENTIFIC RESEARCH LABS SEATTLE WASH GEO-ASTRO PHYSICS LAB
Characteristic times for the cooling of stellar material by spontaneous emission for temperatures between 10 to the 7th power and 10,000K, and for gas pressures corresponding to log P sub g -2 to 4, or alternately, electron densities between 10 to the 8th power and 10 to the 14th powercc are derived. These data are used to predict the time development of an element undergoing a cooling process. The numerical calculations are carried out for equilibrium conditions and continuous emission in an optically thin layer. However, the influences of departures from equilibrium, of line emission, and of finite optical thickness are estimated. The results are applied to a theoretical analysis of relevant flare observations. It is, in particular, shown that on the basis of the above arguments alone a position of the initial flare event in photospheric layers cannot be excluded. Author
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