Observations of solar X-ray bursts in the energy range 5–15 keV |
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| Authors: | Datlowe D W Hudson H S Peterson L E |
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| Institution: | (1) Sacramento Peak Observatory, Air Force Cambridge Research Laboratories, 88349 Sunspot, N.M., U.S.A.;(2) High Altitude Observatory, National Center for Atmospheric Research, 80302 Boulder, Colo., U.S.A. |
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| Abstract: | We simultaneously solve the equations of radiative transfer and statistical equilibrium for a model hydrogen atom including Lyman- , Lyman- , Balmer- and the Lyman, Balmer and Paschen continua. The model atmospheres we use are the results of Nakagawa et al. (1973) for a kinematic model of the chromospheric solar flare.We find that the models adequately predict the total intensity of B, its wing broadening, the presence of a red-shifted wing, the maximum electron density, the total line-of-sight second-level population and the narrowness in height of the B emitting region. The profile of B is strongly self-reversed, however, and agrees with observations only in the presence of 40–70 km s–1 macroturbulent motion.We find that Nakagawa et al. (1973) seriously overestimate the radiative loss function, which will have a large effect on their models. Proper radiative loss calculations must be included in any physically realistic model.The National Center for Atmospheric Research is sponsored by the National Science Foundation. |
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