Modelling a solar flare from X-ray, UV, and radio observations

✍ Scribed by F. Chiuderi Drago; B. C. Monsignori Fossi

• Publisher: Springer
• Year: 1991
• Tongue: English
• Weight: 936 KB
• Volume: 132
• Category: Article
• ISSN: 0038-0938
• DOI: 10.1007/bf00159135

✦ Synopsis

A slowly evolving, flaring loop was observed by the UVSP, XRP, and HXIS instruments onboard SMM on June 10, 1980. Simultaneous radio observations from Toyokawa (Japan) are also available. The SMM instruments have an angular resolution ranging from 3 to 30 arc sec by which the loop structure may be determined. It appears that these observations cannot be accounted for by a single loop model even assuming a variable temperature and pressure. The additional presence of a hot and tenuous isothermal plasma is necessary to explain the harder emission (HXIS). X-ray and UV data are used to fit the differential emission measure as a function of temperature and a model of the flare is deduced, which is then checked against radio data. An estimate of the heating function along the loop and of the total energy content of the loop is also given.