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Dominance of Bursty over Steady Heating of the 4Ė8 MK Coronal Plasma in a Solar Active Region: Quantification Using Maps of Minimum, Maximum, and Average Brightness View all abstracts by submitter

Sanjiv Tiwari   Submitted: 2022-12-28 13:35

A challenge in characterizing active region (AR) coronal heating is in separating transient (bursty) loop heating from the diffuse background (steady) heating. We present a method of quantifying coronal heatingís bursty and steady components in ARs, applying it to Fe XVIII (hot 94) emission of an AR observed by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory. The maximum-, minimum-, and average-brightness values for each pixel, over a 24 hr period, yield a maximum-brightness map, a minimum-brightness map, and an average-brightness map of the AR. Running sets of such three maps come from repeating this process for each time step of running windows of 20, 16, 12, 8, 5, 3, 1, and 0.5 hr. From each running windowís set of three maps, we obtain the ARís three corresponding luminosity light curves. We find (1) the time-averaged ratio of minimum- brightness-map luminosity to average-brightness-map luminosity increases as the time window decreases, and the time-averaged ratio of maximum-brightness-map luminosity to average-brightness-map luminosity decreases as the window decreases; (2) for the 24 hr window, the minimum-brightness mapís luminosity is 5% of the average- brightness mapís luminosity, indicating that at most 5% of the ARís hot 94 luminosity is from heating that is steady for 24 hr; (3) this upper limit on the fraction of the hot 94 luminosity from steady heating increases to 33% for the 30 minute running window. This requires that the heating of the 4Ė8 MK plasma in this AR is mostly in bursts lasting less than 30 minutes: at most a third of the heating is steady for 30 minutes.

Authors: Sanjiv K. Tiwari, Lucy A. Wilkerson, Navdeep K. Panesar, Ronald L. Moore, and Amy R. Winebarger
Projects: SDO-AIA

Publication Status: Published in ApJ
Last Modified: 2023-01-02 23:05
Go to main E-Print page  Solar Orbiter and SDO Observations, and Bifrost MHD Simulations of Small-scale Coronal Jets  Solar flare hard X-rays from the anchor points of an eruptive filament  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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