Physics
Scientific paper
Mar 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982phdt.........3r&link_type=abstract
Ph.D. Thesis California Univ., San Diego.
Physics
14
Chromosphere, Conductive Heat Transfer, Radiative Transfer, Solar Flares, Solar Temperature, Static Models, Equations Of State, Finite Difference Theory, Ionization, Iteration, Solar Electrons
Scientific paper
The response of the solar chromosphere to a long lived flux of nonthermal electrons was modeled of steady state energy balance, radiative transfer, and atomic statistical equilibrium are solved simultaneously by finite difference methods, using linearization and iteration. A semiempirical chromospheric model is assumed as the preflare state. The ambient preflare energy input per atom is deduced from the preflare temperature structure and does not change during the flare heating process. The structure of these chromospheric flare atmospheres shows the difference between the effects of thermal conduction and nonthermal electrons. Only nonthermal electrons cause significant heating below the flare transition region, in the remaining flare chromosphere. Collisional ionization by nonthermal electrons produces noticeable effects on the ionization low in the chromosphere. This, combined with the heating effects of the nonthermal electrons influences the temperature and density there.
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