It is now more than ten years since the first x-ray emitting stellar corona was discovered (Catura, Acton, and Johnson 1975). Since then, rapid progress has been made in cataloging the incidence and range of stellar x-ray emission, most notably with the Einstein Observatory (see, eg., reviews by Ste
Sub-arcsecond observations of the solar X-ray corona
β Scribed by Golub, L.; Herant, M.; Kalata, K.; Lovas, I.; Nystrom, G.; Pardo, F.; Spiller, E.; Wilczynski, J.
- Book ID
- 109763342
- Publisher
- Nature Publishing Group
- Year
- 1990
- Tongue
- English
- Weight
- 629 KB
- Volume
- 344
- Category
- Article
- ISSN
- 0028-0836
- DOI
- 10.1038/344842a0
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The soft X-ray emission of the solar corona is investigated by comparison of the signals of several broad band photometers carried on the Solrad 9 satellite, and sensitive to the region 0.5-20 A. Temperature from 1.5 β’ 106 to 25 β’ 106 K have been measured with 'emission measure' S N~2 dVranging betw
Several problems related to the calculation of an emission measure differential in temperature are resolved using a new calculation technique. The analysis of a flare on 20 April, 1976, is used to evaluate the usefulness of this new approach and to estimate its future value.