An analysis of the growth of X-ray loops in the flare of 21 May, 1980, observed by HXI S on board SMM spacecraft, has been carried out with high time resolution in six energy channels from 3.5 to 30 keV. This analysis has revealed that the tops of the loops stay for minutes at a given altitude befor
X-ray observations of filament eruption in the 1980 May 21 flare
β Scribed by D. A. Batchelor; K. P. Hindsley
- Publisher
- Springer
- Year
- 1991
- Tongue
- English
- Weight
- 811 KB
- Volume
- 135
- Category
- Article
- ISSN
- 0038-0938
No coin nor oath required. For personal study only.
π SIMILAR VOLUMES
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 β’ 10 -8 ergscm-es
Gradual enhancements which repeatedly appeared 20-50 min after the onset of an impulsive burst were observed in microwaves and hard X-rays. The observed characteristics of the gradual enhancements are (i) the similarity of time profiles in both the frequency range of 17 GHz to 160 MHz and the energ
as well as improved parameters for the OSO-4 instrument. These will be published in a subsequent communication.