Nonequilibrium ionization effects in asymmetrically heated loops

Details Nonequilibrium ionization effects in asymmetrically heated loops Nonequilibrium ionization effects in asymmetrically heated loops

Nov 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...382..338s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 382, Nov. 20, 1991, p. 338-343. Research supported by U.S. Navy and NASA.

Physics

26

Late Stars, Nonequilibrium Ionization, Radiative Heat Transfer, Solar Prominences, Carbon, Doppler Effect, Emission Spectra, Extreme Ultraviolet Radiation, Oxygen Ions, Plasmas (Physics), Red Shift, Solar Corona

Scientific paper

The effects of nonequilibrium ionization on magnetic loop models with a steady siphon flow that is driven by a nonuniform heating rate are investigated. The model developed by Mariska (1988) to explain the observed redshifts of transition region emission lines is examined, and the number densities of the ions of carbon and oxygen along the loop are computed, with and without the approximation of ionization equilibrium. Considerable deviations from equilibrium were found. In order to determine the consequences of these nonequilibrium effects on the characteristics of the EUV emission from the loop plasma, the profiles and wavelength positions of all the important emission lines due to carbon and oxygen were calculated. The calculations are in broad agreement with Mariska's conclusions, although they show a significant diminution of the Doppler shifts, as well as modifications to the line widths. It is concluded that the inclusion of nonequilibrium effects make it more difficult to reproduce the observed characteristics of the solar transition region by means of the asymmetric-heating models.

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