Determining the Nanoflare Heating Frequency of an X-Ray Bright Point Observed by MaGIXS

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dc.citation.articleNumber23en_US
dc.citation.journalTitleThe Astrophysical Journalen_US
dc.citation.volumeNumber967en_US
dc.contributor.authorMondal, Biswajiten_US
dc.contributor.authorAthiray, P. S.en_US
dc.contributor.authorWinebarger, Amy R.en_US
dc.contributor.authorSavage, Sabrina L.en_US
dc.contributor.authorKobayashi, Kenen_US
dc.contributor.authorBradshaw, Stephenen_US
dc.contributor.authorBarnes, Willen_US
dc.contributor.authorChampey, Patrick R.en_US
dc.contributor.authorCheimets, Peteren_US
dc.contributor.authorDudík, Jaroslaven_US
dc.contributor.authorGolub, Leonen_US
dc.contributor.authorMason, Helen E.en_US
dc.contributor.authorMcKenzie, David E.en_US
dc.contributor.authorMoore, Christopher S.en_US
dc.contributor.authorMadsen, Chaden_US
dc.contributor.authorReeves, Katharine K.en_US
dc.contributor.authorTesta, Paolaen_US
dc.contributor.authorVigil, Genevieve D.en_US
dc.contributor.authorWarren, Harry P.en_US
dc.contributor.authorWalsh, Robert W.en_US
dc.contributor.authorZanna, Giulio Delen_US
dc.date.accessioned2024-08-07T19:15:00Zen_US
dc.date.available2024-08-07T19:15:00Zen_US
dc.date.issued2024en_US
dc.description.abstractNanoflares 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.en_US
dc.identifier.citationMondal, B., Athiray, P. S., Winebarger, A. R., Savage, S. L., Kobayashi, K., Bradshaw, S., Barnes, W., Champey, P. R., Cheimets, P., Dudík, J., Golub, L., Mason, H. E., McKenzie, D. E., Moore, C. S., Madsen, C., Reeves, K. K., Testa, P., Vigil, G. D., Warren, H. P., … Zanna, G. D. (2024). Determining the Nanoflare Heating Frequency of an X-Ray Bright Point Observed by MaGIXS. The Astrophysical Journal, 967(1), 23. https://doi.org/10.3847/1538-4357/ad2766en_US
dc.identifier.digitalMondal_2024_ApJ_967_23en_US
dc.identifier.doihttps://doi.org/10.3847/1538-4357/ad2766en_US
dc.identifier.urihttps://hdl.handle.net/1911/117600en_US
dc.language.isoengen_US
dc.publisherIOP Publishingen_US
dc.rightsExcept where otherwise noted, this work is licensed under a Creative Commons Attribution (CC BY) license.  Permission to reuse, publish, or reproduce the work beyond the terms of the license or beyond the bounds of fair use or other exemptions to copyright law must be obtained from the copyright holder.en_US
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/en_US
dc.titleDetermining the Nanoflare Heating Frequency of an X-Ray Bright Point Observed by MaGIXSen_US
dc.typeJournal articleen_US
dc.type.dcmiTexten_US
dc.type.publicationpublisher versionen_US
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