Abstract
The burst component of the solar X-ray flux in the soft wavelength range 2 < λ < 12 Å observed from Explorer 33 and Explorer 35 from July 1966 to September 1968 was analyzed. In this period 4028 burst peaks were identified.
The differential distributions of the temporal and intensity parameters of the bursts revealed no separation into more than one class of bursts. The most frequently observed value for rise time was 4 min and for decay time was 12 min. The distribution of the ratio of rise to decay time can be represented by an exponential with exponent -2.31 from a ratio of 0.3 to 2.7; the maximum in this distribution occurred at a ratio of 0.3. The values of the total observed flux, divided by the background flux at burst maximum, can be represented by a power law with exponent -2.62 for ratios between 1.5 and 32. The distribution of peak burst fluxes can be represented by a power law with exponent - 1.75 over the range 1–100 milli-erg (cm2 sec)−1. The flux time integral values are given by a power law with exponent -1.44 over the range 1–50 erg cm−2.
The distribution of peak burst flux as a function of Hα importance revealed a general tendency for larger peak X-ray fluxes to occur with both larger Hα flare areas and with brighter Hα flares. There is no significant dependence of X-ray burst occurrence on heliographic longitude; the emission thus lacks directivity.
The theory of free-free emission by a thermal electron distribution was applied to a composite quantitative discussion of hard X-ray fluxes (data from Arnoldy et al., 1968; Kane and Winckler, 1969; and Hudson et al., 1969) and soft X-ray fluxes during solar X-ray bursts. Using bursts yielding measured X-ray intensities in three different energy intervals, covering a total range of 1–50 keV, temperatures and emission measures were derived. The emission measure was found to vary from event to event. The peak time of hard X-ray events was found to occur an average of 3 min before the peak time of the corresponding soft X-ray bursts. Thus a changing emission measure during the event is also required. A free-free emission process with temperatures of 12–39 × 106K and with an emission measure in the range 3.6 × 1047 to 2.1 × 1050 cm−3 which varies both from event to event and within an individual event is required by the data examined.
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Now at Department of Astrophysical Sciences, Princeton University, Princeton, New Jersey.
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Drake, J.F. Characteristics of soft solar X-ray bursts. Sol Phys 16, 152–185 (1971). https://doi.org/10.1007/BF00154510
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DOI: https://doi.org/10.1007/BF00154510