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Constraining Nanoflare Frequency Through Observations and ModelsNanoflares are considered prime candidates for heating the non-flaring solar corona. However, direct detection of individual nanoflares with present-generation instruments remains challenging. Understanding the frequency and magnitude of nanoflares is crucial for comprehending their role in coronal heating. In this study, we employ field-aligned hydrodynamic model to simulate the emission from a non-flaring X-ray bright point (XBP) observed by the Marshall Grazing Incidence X-ray Spectrometer (MaGIXS). The length and magnetic field strength of the coronal loops associated with this XBP are derived from magnetic field extrapolation of observed photospheric magnetograms by SDO/HMI. Each loop is assumed to be heated by random nanoflares, whose frequency and magnitude are determined by the loop length and their field strength. The simulation results are then compared and matched against the observation to determine the nanoflare heating frequency. We will discuss the findings of this study. Furthermore, we will discuss the evolution of nanoflare heating frequency during the formation and decay of an active region (AR) on the solar disk.
Document ID
20240007673
Acquisition Source
Marshall Space Flight Center
Document Type
Presentation
Authors
Biswajit Mondal
(Marshall Space Flight Center Redstone Arsenal, United States)
Amy Renee Winebarger
(Marshall Space Flight Center Redstone Arsenal, United States)
Date Acquired
June 15, 2024
Subject Category
Solar Physics
Meeting Information
Meeting: Talk at Max Planck Institute for Solar System Research
Location: Göttingen
Country: DE
Start Date: June 20, 2024
Sponsors: American Geophysical Union
Funding Number(s)
WBS: 791926.02.19.01.07
Distribution Limits
Public
Copyright
Public Use Permitted.
Keywords
coronalheating
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