Flare loop radiative hydrodynamics. III - Nonlocal radiative transfer effects

Details Flare loop radiative hydrodynamics. III - Nonlocal radiative transfer effects Flare loop radiative hydrodynamics. III - Nonlocal radiative transfer effects

Feb 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...265..507c&link_type=abstract

Astrophysical Journal, Part 1, vol 265, Feb. 1, 1983, p. 507-518.

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8

Chromosphere, Magnetohydrodynamics, Radiative Transfer, Solar Atmosphere, Solar Flares, Solar Spectra, Atmospheric Models, H Lines, Hydrogen Ions, Line Spectra, Optical Thickness, Solar Temperature, Thermal Stability

Scientific paper

The study has three goals. The first is to demonstrate that processes exist whose intrinsic nonlocal nature cannot be represented by local approximations. The second is to elucidate the physical nature and origins of these nonlocal processes. The third is to suggest that the methods and results described here may prove useful in constructing semiempirical models of the chromosphere by means more efficient than trial and error. Matrices are computed that describe the effect of a temperature perturbation at an arbitrary point in the loop on density, hydrogen ionized fraction, total radiative loss rate, and radiative loss rate of selected hydrogen lines and continua at all other points. It is found that the dominant nonlocal radiative transfer effects can be separated into flux divergence coefficient effects and upper level population effects. The former are most important when the perturbation takes place in a region of significant opacity. Upper level population effects arise in both optically thick and thin regions in response to nonlocal density, ionization, and interlocking effects.

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