Characteristics of the impulsive X-ray component are deduced from thirteen bursts of hard (>10 keV) X-rays observed with the OGO-5 satellite during the period 1968 Iarch 2 1-June 30. Iost of these impulsive X-ray bursts were associated with impulsive microwave bursts and optical flares of importance <1. For 40 keV X-rays the c-folding rise time and decay time are found to be 2-5 and 3-10 sec, . At maximum intensity the X-ray spectrum is consistent with the form photons sec ' keV ', where 2.7 < < 4.5 and 10 < E < 70 keV. The peak X-ray flux above 10 keV observed at the Earth was -` - ergs Under the assumption that electron-proton bremsstrahlung is the mechanism for X-ray production, the spectrum of the energetic electrons in the X-ray source region has been deduced and is found to be consistent with the form ` electrons , where 1.5 < <3.3 and 10 10 keV are a nonthermal flash-phase phenomenon. There is evidence that the injection of energetic electrons into the X-ray source region occurs more or less continuously throughout the implusive X-ray burst. This injection, combined with the loss of energetic electrons through escape and collisions, probably determines the time-intensity profile of an impulsive X-ray burst.
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Kane et al. (1970) studied this question.