Theoretical Study of the Spatially Resolved Soft X-Ray versus Hard X-Ray Relationship in Solar Flares

Details Theoretical Study of the Spatially Resolved Soft X-Ray versus Hard X-Ray Relationship in Solar Flares Theoretical Study of the Spatially Resolved Soft X-Ray versus Hard X-Ray Relationship in Solar Flares

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...491..395l&link_type=abstract

Astrophysical Journal v.491, p.395

Astronomy and Astrophysics

Astronomy

5

Sun: Flares, Sun: X-Rays, Gamma Rays

Scientific paper

We have carried out a series of calculations of the hard (>30 keV) and soft (1-3 keV) X-ray time histories for various parts of a solar flare loop using hydrodynamic simulations of the electron-heated flare atmosphere. We have considered two typical cases: the strongly evaporated flare in which the injected energetic electron flux is large and the initial atmospheric density is small, and the weakly evaporated flare in which the electron flux is small and the initial atmospheric density is large. The spatially unresolved Neupert effect that the time derivative of the soft X-ray time history is proportional to the hard X-ray time history holds for these models; however, in both cases, we find that the footpoint soft X-ray time history is not proportional to the hard X-ray time history at the same location. The model cannot explain recent observations in which a correlation between the soft and hard X-ray time histories (and not a "derivative" relation) at the flare footpoint was observed. Furthermore, the loop-top soft X-ray source decays much earlier than indicated by observations. In order for these model predictions to be consistent with observations, the footpoint soft X-ray source may have to be nonthermal, excited by low-energy electrons. Also, continuous heating of the plasma at the top of the loop is required in addition to that from energetic electrons.

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