Energetic Ions Accelerated during the large solar flare of 24 May 1990: high energy gamma-ray observations

Details Energetic Ions Accelerated during the large solar flare of 24 May 1990: high energy gamma-ray observations Energetic Ions Accelerated during the large solar flare of 24 May 1990: high energy gamma-ray observations

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh32b..08v&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH32B-08

Physics

7514 Energetic Particles (2114), 7519 Flares, 7554 X Rays, Gamma Rays, And Neutrinos

Scientific paper

The large flare of 24 May 1990 (GOES X9.3, N36 W76) was observed at X-ray/gamma-ray energies by PHEBUS aboard GRANAT (Talon et al., 1993, Solar Phys., 147,137) and described in detail in Debrunner et al., 1997 (ApJ, 479,997). The flare comprised an impulsive phase detected at gamma-ray energies up to 75 MeV, followed by a long duration tail at high energies. The long lasting emission was dominated by high energy gamma-ray continuum and by > 500 MeV neutrons. Here we combine the observations of the gamma-ray continuum in the 10-100 MeV photon energy range with calculations of pion-decay gamma-ray radiation to constrain the accelerated interacting ion distributions at energies above 300 MeV. We compare this information with the numbers previously obtained for this event (Debrunner et al., 1997), for ions above 30 MeV from the de-excitation gamma-ray line emission as well as from the observations of neutrons from ground-based monitors. We find that the complete set of gamma-ray observations cannot be reproduced with a single power law ion spectrum extending from gamma-ray line emitting energies to those characteristic of pion decay emission. Similar ion energy distribution behaviour has been reported for the energetic flare of 15 June 1991, and we discuss our results in the light of this previous finding. Finally we comment on the different characteristics found for interacting and escaping protons.

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