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Nonthermal Processes in Large Solar Flares

Published online by Cambridge University Press:  14 August 2015

H. S. Hudson ,
T. W. Jones  and
R. P. Lin
H. S. Hudson
Affiliation:
Physics Dept., University of California, San Diego, La Jolla, Calif., U.S.A.
T. W. Jones
Affiliation:
Physics Dept., University of California, San Diego, La Jolla, Calif., U.S.A.
R. P. Lin
Affiliation:
Space Sciences Laboratory, University of California, Berkeley, Calif. U.S.A.

Summary

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In many small solar flares the ∼10–100 keV electrons accelerated during the flash phase contain the bulk of the total flare energy output. In large flares, such as those in the period 1972, August 2–7, the flash phase electrons are present in substantially greater numbers. These electrons can explosively heat the chromosphere-lower corona and eject flare material. The ejected matter can produce a shock wave which will then accelerate nucleons and electrons to relativistic energies. We analyze energetic particle, radio, X-ray, gamma ray and interplanetary shock observations of the 1972 August flares to obtain quantitative estimates of the energy contained in each facet of these large flares. In general these observations are consistent with the above hypothesis. In particular:

  1. (1) From the X-ray emission (van Beek et al., 1973) the energy contained in >25 keV electrons is calculated to be 2 × 1032 erg for the 1972, August 4 event. Since the lower energy cutoff to the electron spectrum is known to be below 25 keV and possibly below 10 keV, the electrons contain enough energy to produce the following interplanetary shock wave, which has by far the bulk of the energy dissipated in the flare. Similar numbers are obtained for the large August 7 flare event.

  2. (2) From the γ-ray emission (Chupp et al., 1973) the energy in protons dumped at the same level of the atmosphere, assuming a thick target situation, is at least a factor of three smaller than the electrons. Moreover the γ-ray emission indicates that the bulk of the protons are accelerated at least several minutes after the electrons. Thus it is more likely that the electrons are responsible for the flare optical (Hα and white light) emissions which occur in the chromosphere.

  3. (3) Approximately 5% of the electrons and 99% of the protons escape into the interplanetary medium to be observed by spacecraft. This situation is consistent with the hypothesis of shock acceleration of the protons high in the solar corona.

  4. (4) The four most intense X-ray bursts observed during the period July 31–August 11 are the only bursts followed by an interplanetary shock wave and a new injection of energetic protons into the interplanetary medium.

Type
Part 3: Solar Flares
Information
Symposium - International Astronomical Union , Volume 68: Solar X, Gamma, and EUV Radiation , 1975 , pp. 425 - 426
Copyright
Copyright © Reidel 1975 

References

Chupp, E. L., Forrest, D. J., and Suri, A. N.: 1973, in Ramaty, R. and Stone, R. G. (eds.), High Energy Phenomena on the Sun, NASA SP-342, p. 285.Google Scholar
Van Beek, H. F., Hoyng, P., and Stevens, G. A.: 1973, in Coffey, H. E. (ed.), Collected Data Reports on the August 1972 Solar-Terrestrial Events, UAG-28, Part II, p. 319.Google Scholar