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On fine structure in solar flares observed from SDO, RHESSI, and TRACEтезисы доклада
- Авторы: Porfir`eva G.A., Yakunina G.V.
- Сборник: Тезисы на сайте конфеенции http://ws-sozopol.stil.bas.bg/
- Серия: Nessebar, Bulgaria
- Тезисы
- Год издания: 2013
- Место издания: Nessebar, Bulgaria
- Первая страница: 1
- Аннотация: Results of spatially and temporally resolved observations of several solar fares are considered. Images, obtained simultaneously in optical, UV, EUV, soft and hard X-rays, demonstrate complexity and variability of composite flare structures. Flaring plasma seems to be confined to fine multiple coronal loops. The volume of a flare extends from the uppermost photosphere throughout the chromosphere and transition region up to low corona. Analysis of observations shows height temperature stratification in a solar flare. High temperature (TЎЭ2 MK) hard X-ray emission originates on lower atmosphere layers while lower temperature (T<2 MK) soft X-ray and EUV emission originates higher (above the chromoshere) and white-light continuum is formed in upper chromosphere powered by low energy electrons. Observations have revealed that multiple magnetic reconnection occur simultaneously at different sites changing their locations inside the flare volume with time. Some simulations of observed processes are discussed. Data from Internet and published scientific papers have been used.
- Добавил в систему: Якунина Галина Валентиновна