Abstract The study of physical conditions and the geometry of solar coronal structures is a subject of substantial interest among the solar physics community. In the present review the new methods are presented allowing for identification of so called Non-Equilibrium and Quasi-Steady-State phases during the evolution of the flare, based on the soft X-ray observations. Identification of the Quasi-Steady-State phase in the observed flares allows to relate the plasma parameters with the effective geometrical characteristics of the flaring loops. Next, the comparison with the observed flaring loop sizes allows to investigate the heating rate of the plasma and the plasma density. Arguments are presented showing validity of the heating rate diagnostics also for the initial Non-Equilibrium flare phase. This, in turn, provides an important diagnostic tool for studying the flare energy balance during the initial phase. Results of the hydrodynamic flaring loop model calculations confirm usefulness of the energy balance analysis method for investigation of flares during the initial phase. Presented methods have large potential possibilities of further improvement and they should be used more efficiently in future studies.
Coronal loops, X-ray diagnostics
Advances in Space Research ; 8 , 11 ; 55-66
1989-01-01
12 pages
Article (Journal)
Electronic Resource
English
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