Dynamics of an atmosphere irradiated by soft X-rays in flares

Details Dynamics of an atmosphere irradiated by soft X-rays in flares Dynamics of an atmosphere irradiated by soft X-rays in flares

Jun 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978a%26a....66..385h&link_type=abstract

Astronomy and Astrophysics, vol. 66, no. 3, June 1978, p. 385-393.

Astronomy and Astrophysics

Astrophysics

16

Atmospheric Heating, Chromosphere, Plasma-Electromagnetic Interaction, Solar Atmosphere, Solar Flares, Solar X-Rays, X Ray Irradiation, Boundary Value Problems, Energy Dissipation, Radiative Transfer, Solar Corona, Stellar Models

Scientific paper

It was previously shown that the lower chromosphere can be heated substantially by soft X-ray radiation at wavelengths of 1-300 A arising from a high-temperature plasma in the corona during a flare. The analysis was, however, based on the steady-state approximation. In this paper, a more realistic dynamic response is examined utilizing numerical calculations. Specifically, the physical parameters, such as the temperature, emission measure, and physical size of the X-ray source, are taken similar to the previous study; i.e., typical values for one 1N flares. The initial atmosphere is represented by the HSRA model atmosphere. The results indicate that with continuous and constant irradiation by the soft X-ray flux: (1) the atmosphere undergoes an oscillating expansion characterized by an oscillation period of approximately 270 s before reaching a new steady state in about 30 min; (2) in the oscillatory motions, a temperature increase coincides with downward motions and with upward motions; and (3) the observed time variation of the H-alpha line profile in flares appears to be in agreement with the initial part of the oscillatory behavior. It is noted that the oscillatory motions may not arise for spatially as well as temporally inhomogeneous soft X-ray sources.

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