A new series of solar flare energetic X-ray events has been detected by an ionization chamber on the OGO-I and OGO-III satellites in free space. These X-rays lie in the range 10-50 keV, and a study has been made of their relationship to 3 and 10 cm radio bursts and with the emission of electrons and
Cyclic distribution of energetic X-ray flares
โ Scribed by T. Landscheidt
- Publisher
- Springer
- Year
- 1986
- Tongue
- English
- Weight
- 279 KB
- Volume
- 107
- Category
- Article
- ISSN
- 0038-0938
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โฆ Synopsis
The Blackman-Tukey power spectrum of flare generated X-ray bursts > X 1 observed from 1970 to 1982 by satellite instrumentation (SOLRAD/SMS/GOES) shows prominent peaks at 156, 4.8, 2.8, and 1.1 months. According to a statistical test of the significance of the deviation of these peaks from Markov red noise, the peaks at 2.8 and 1.1 months are significant at the 99% confidence level while the peak at 4.8 months reaches the 95 % level. A replication by means of the maximum entropy spectral analysis (MEM) yields the same prominent peaks at the same frequencies.
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On 23 May 1967 energetic (10-50 kcV) solar flare X-rays were observed by the OGO-III ion chamber during the period 1808-2100 UT. The time-intensity profile for the X-ray event showed three distinct pcaks at ~: 1810, 1841 and 1942 UT. The second peak, which is eqtfivalent to ~-: 2.9 โข 10 -8 ergscm-es
This paper presents studies of the vertical structure of hard X-ray flares for two contrasting examples. The 1981 May 13 flare contained a coronal hard X-ray source which was located above 50000 km above the photosphere. On the other hand, the 1981 July 20 flare had a chromospheric double source str