The Flare Emission of the May 4, 2022 Event and Its Millimeter Component
Identifikátory výsledku
Kód výsledku v IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F23%3A00580089" target="_blank" >RIV/67985815:_____/23:00580089 - isvavai.cz</a>
Výsledek na webu
<a href="https://doi.org/10.1134/S0016793223600558" target="_blank" >https://doi.org/10.1134/S0016793223600558</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1134/S0016793223600558" target="_blank" >10.1134/S0016793223600558</a>
Alternativní jazyky
Jazyk výsledku
angličtina
Název v původním jazyce
The Flare Emission of the May 4, 2022 Event and Its Millimeter Component
Popis výsledku v původním jazyce
Based on observations at the RT-7.5 radio telescope of the Bauman Moscow State Technical University at a wavelength of 3.2 mm (93 GHz), along with other ground-based and space instruments (Siberian Radioheliograph, Solar Dynamics Observatory (SDO), Metsähovi Radio Observatory), the origin of millimeter radiation from X-ray class M 5.7 SOL2022-05-04T08:45 solar flare was investigated. An analysis of the time profiles of radiation in the X-ray and radio ranges showed that the millimeter emission source is not associated with hot (5 × 105-107 K) coronal plasma. This is also evidenced by the estimate of the sub-THz flux from radiating hot plasma according to the AIA/SDO data, which turned out to be much less than the observed values. Indications of the development of thermal instability in flare ultraviolet loops were obtained. The relationship between the millimeter emission of the flare and the heat source in the solar chromosphere has been substantiated.
Název v anglickém jazyce
The Flare Emission of the May 4, 2022 Event and Its Millimeter Component
Popis výsledku anglicky
Based on observations at the RT-7.5 radio telescope of the Bauman Moscow State Technical University at a wavelength of 3.2 mm (93 GHz), along with other ground-based and space instruments (Siberian Radioheliograph, Solar Dynamics Observatory (SDO), Metsähovi Radio Observatory), the origin of millimeter radiation from X-ray class M 5.7 SOL2022-05-04T08:45 solar flare was investigated. An analysis of the time profiles of radiation in the X-ray and radio ranges showed that the millimeter emission source is not associated with hot (5 × 105-107 K) coronal plasma. This is also evidenced by the estimate of the sub-THz flux from radiating hot plasma according to the AIA/SDO data, which turned out to be much less than the observed values. Indications of the development of thermal instability in flare ultraviolet loops were obtained. The relationship between the millimeter emission of the flare and the heat source in the solar chromosphere has been substantiated.
Klasifikace
Druh
J<sub>imp</sub> - Článek v periodiku v databázi Web of Science
CEP obor
—
OECD FORD obor
10308 - Astronomy (including astrophysics,space science)
Návaznosti výsledku
Projekt
Výsledek vznikl pri realizaci vícero projektů. Více informací v záložce Projekty.
Návaznosti
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Ostatní
Rok uplatnění
2023
Kód důvěrnosti údajů
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Údaje specifické pro druh výsledku
Název periodika
Geomagnetism and Aeronomy
ISSN
0016-7932
e-ISSN
1555-645X
Svazek periodika
63
Číslo periodika v rámci svazku
5
Stát vydavatele periodika
RU - Ruská federace
Počet stran výsledku
9
Strana od-do
527-535
Kód UT WoS článku
001088700200002
EID výsledku v databázi Scopus
2-s2.0-85174181149