Accelerated Electrons in the 27 June 1980 Solar Flare

Details Accelerated Electrons in the 27 June 1980 Solar Flare Accelerated Electrons in the 27 June 1980 Solar Flare

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.3016j&link_type=abstract

American Astronomical Society, 180th AAS Meeting, #30.16; Bulletin of the American Astronomical Society, Vol. 24, p.778

Astronomy and Astrophysics

Astronomy

1

Scientific paper

We analyze hard X-ray measurements of a solar flare which occured on 27 June 1980. The data were taken by the balloon borne HIREX germanium spectrometer. The spectrometer has a resolution ~ 1 keV. The flare as observed in hard X-rays lasted 3 minutes. The data are binned into 5 second intervals. The hard X-ray spectrum of each interval is then deconvolved according to the procedure of Johns and Lin (1992) to find the instantaneous X-ray emitting population of electrons. A continuity equation is then used to find the spectrum (total number per unit energy per unit time) of accelerated electrons at each time step in the flare event. The continuity equation only includes energy losses by Coulomb collisions. The result thus obtained is independent of the volume and nearly independent of the density of the X-ray emitting region. The spectrum of accelerated electrons can then be integrated over energy and time to obtain a lower limit on the the total energy of accelerated electrons produced during the flare. The estimate is a lower limit since we only operate on the observed portion of the hard X-ray spectrum, taking care not to include the contribution of the superhot component. The total energy of electrons with E > 20 keV in the 27 June 1980 flare is found to be E=2.54 +/- 0.06 times 10(30) ergs assuming the electrons lose the majority of their energy in a fully ionized plasma. The derived energy depends on whether the electrons lose their energy in an ionized or neutral medium. If the region is neutral then the flare energy in hard X-rays is E=1.09 +/- 0.03 times 10(30) ergs. We will also discuss the shape of the accelerated electron spectrum as a function of time in the flare and what constraints on acceleration mechanisms this information contains. Johns, C.M. and Lin, R.P. 1992, Sol. Phys., 137, 121.

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