Počet záznamů: 1
Determining the nanoflare heating frequency of an X-ray bright point observed by MaGIXS
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SYSNO ASEP 0586241 Druh ASEP J - Článek v odborném periodiku Zařazení RIV J - Článek v odborném periodiku Poddruh J Článek ve WOS Název Determining the nanoflare heating frequency of an X-ray bright point observed by MaGIXS Tvůrce(i) Mondal, B. (US)
Athiray, P. S. (US)
Winebarger, A. (US)
Dudík, Jaroslav (ASU-R) RID, ORCIDCelkový počet autorů 21 Číslo článku 23 Zdroj.dok. Astrophysical Journal - ISSN 0004-637X
Roč. 967, č. 1 (2024)Poč.str. 12 s. Forma vydání Online - E Jazyk dok. eng - angličtina Země vyd. GB - Velká Británie Klíč. slova solar coronal heating ; solar coronal loops ; solar x-ray emission Obor OECD Astronomy (including astrophysics,space science) Způsob publikování Open access Institucionální podpora ASU-R - RVO:67985815 UT WOS 001222070000001 EID SCOPUS 85193053819 DOI https://doi.org/10.3847/1538-4357/ad2766 Anotace Nanoflares are thought to be one of the prime candidates that can heat the solar corona to its multimillion kelvin temperature. Individual nanoflares are difficult to detect with the present generation of instruments, but their presence can be inferred by comparing simulated nanoflare-heated plasma emissions with the observed emission. Using HYDRAD coronal loop simulations, we model the emission from an X-ray bright point (XBP) observed by the Marshall Grazing Incidence X-ray Spectrometer (MaGIXS), along with the nearest available observations from the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) and the X-Ray Telescope (XRT) on board the Hinode observatory. The length and magnetic field strength of the coronal loops are derived from the linear force-free extrapolation of the observed photospheric magnetogram by the Helioseismic and Magnetic Imager on board SDO. Each loop is assumed to be heated by random nanoflares, whose magnitude and frequency are determined by the loop length and magnetic field strength. The simulation results are then compared and matched against the measured intensity from AIA, XRT, and MaGIXS. Our model results indicate the observed emission from the XBP under study could be well matched by a distribution of nanoflares with average delay times 1500-3000 s. Further, we demonstrate the high sensitivity of MaGIXS and XRT for diagnosing the heating frequency using this method, while AIA passbands are found to be the least sensitive. Pracoviště Astronomický ústav Kontakt Anežka Melichárková, bibl@asu.cas.cz, Tel.: 323 620 326 Rok sběru 2025 Elektronická adresa https://hdl.handle.net/11104/0354011
Počet záznamů: 1