Solar flares are common and strong demonstrations of solar activity. They are observable throughout the whole electromagnetic spectrum. If they show a broadband emission in the visible continuum, then we speak of white-light flares. The origin of white-light flares is not fully understood. We detected 24 white-light flares in SDO/HMI data and analyzed them using SDO/AIA wavelength bands at 1 700 ̊A and 304 ̊A and GONG Hα observations. According to our work, the emission in the 1 700 ̊A band is similar to the white-light emission but usually starts sooner. The positions of intensity enhancements in the 1 700 ̊A band are similar to the positions of the white-light flares and are connected by ribbons visible in the 304 ̊A band and in the Hα line. Then we studied the decay time of white-light flares and found that for most of the white-light flare points the typical decay time ranges in 2 - 3 min. 1
| Identifer | oai:union.ndltd.org:nusl.cz/oai:invenio.nusl.cz:398089 |
| Date | January 2019 |
| Creators | Mravcová, Lucia |
| Contributors | Švanda, Michal, Zemanová, Alena |
| Source Sets | Czech ETDs |
| Language | English |
| Detected Language | English |
| Type | info:eu-repo/semantics/masterThesis |
| Rights | info:eu-repo/semantics/restrictedAccess |
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