Time delays in large and small loop thermal models for hard X-ray bursts

Details Time delays in large and small loop thermal models for hard X-ray bursts Time delays in large and small loop thermal models for hard X-ray bursts

Jan 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984soph...90...83s&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 90, Jan. 1984, p. 83-96.

Physics

5

Coronal Loops, Solar Flares, Solar X-Rays, Bursts, Conductive Heat Transfer, Electron Energy, Plasma Heating, Solar Electrons, Solar Temperature, Spatial Distribution, Time Lag, X Ray Spectra

Scientific paper

The time histories of the emission at 10, 30, and 100 keV averaged over the loop from small and large loop thermal models of hard X-ray emission are studied. The small (15,000 km) loop cases show a characteristic delay in the peak of the 100 keV emission relative to the 30 keV emission of about 1.5 s which should be detectable. The large (47,000 km) loop cases show no delay, but in the case of a continuous energy input, the 30 keV emission has a peak at 9.5 s whereas the 100 keV emission rises monotonically. A large loop case where only classical and saturated heat conduction is allowed is considered. The 30 keV emission has a peak at 7.5 s whereas the 100 keV emission rises monotonically. The peak temperature reached is 8 x 10 to the 7th K and the probability of finding examples in the data uncontaminated by a dominant beam or escaping tail component should be considerably higher than in the cases with higher rates of energy input.

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