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Simulation of Subterahertz Emission from the April 2, 2017 Solar Flare Based on the Multiwavelength Observations
Tekijät: Morgachev AS, Tsap YT, Smirnova VV, Motorina GG
Kustantaja: MAIK NAUKA/INTERPERIODICA/SPRINGER
Julkaisuvuosi: 2018
Lehti:: Geomagnetism and Aeronomy
Tietokannassa oleva lehden nimi: GEOMAGNETISM AND AERONOMY
Lehden akronyymi: GEOMAGN AERONOMY+
Vuosikerta: 58
Numero: 8
Aloitussivu: 1113
Lopetussivu: 1122
Sivujen määrä: 10
ISSN: 0016-7932
eISSN: 1555-645X
DOI: https://doi.org/10.1134/S001679321808011X
Tiivistelmä
Millimeter (93 and 140 GHz) emission of the M6.4 solar flare detected on April 2, 2017 in the NOAA 12644 active region by the RT-7.5 telescope of the Bauman Moscow State Technical University is analyzed using the observational data provided by the Radio Solar Telescope Network (4.9, 8.8, and 15.4GHz); the SDO/AIA satellites (Etreme Ultraviolet); and GOES, RHESSI, and Konus-Wind (X-rays). It is found that the spectral flux density of millimeter emission increases with frequency throughout the entire burst. The similarity between the profiles of millimeter and soft-X-ray radiation suggests that the burst is of a thermal nature. It follows from the results of calculations of the differential emission measure of coronal plasma based on the SDO/AIA data that its contribution to millimeter emission of the flare is negligible. The simulation of thermal emission of chromospheric flare plasma in the model of Machado (Machado et al., 1980) yields millimeter fluxes that are by several times lower than the observed ones. The physical implications of these results are discussed.
Millimeter (93 and 140 GHz) emission of the M6.4 solar flare detected on April 2, 2017 in the NOAA 12644 active region by the RT-7.5 telescope of the Bauman Moscow State Technical University is analyzed using the observational data provided by the Radio Solar Telescope Network (4.9, 8.8, and 15.4GHz); the SDO/AIA satellites (Etreme Ultraviolet); and GOES, RHESSI, and Konus-Wind (X-rays). It is found that the spectral flux density of millimeter emission increases with frequency throughout the entire burst. The similarity between the profiles of millimeter and soft-X-ray radiation suggests that the burst is of a thermal nature. It follows from the results of calculations of the differential emission measure of coronal plasma based on the SDO/AIA data that its contribution to millimeter emission of the flare is negligible. The simulation of thermal emission of chromospheric flare plasma in the model of Machado (Machado et al., 1980) yields millimeter fluxes that are by several times lower than the observed ones. The physical implications of these results are discussed.
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