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Investigation of Heating of Active Region Coronal Loops in non-Eruptive Solar Active Regions

Presentation #105.08 in the session Ambient Solar Atmosphere Posters.

Published onSep 18, 2023
Investigation of Heating of Active Region Coronal Loops in non-Eruptive Solar Active Regions

Based on the results from Tiwari et al. 2017, we investigate the importance of magneto-convection in heating active region coronal loops. Tiwari et al. found via SDO/AIA observations and NLFFF extrapolations that loops connecting sunspot umbrae are invisible in EUV images and those with one loop footpoint in sunspot umbra or penumbra and the other footpoint in opposite-polarity sunspot penumbra or plage regions, are seen as bright and hot loops. They conclude that a combination of the magnetic field strength of the regions the loops are rooted in and the convective freedom of the regions play an important role in determining the amount of heating in these loops.

The aim of our present study is to understand the statistical significance of the above findings. We select a sample of active regions of three kinds: 1. those containing a pair of sunspots, 2. those with a sunspot in the leading polarity but not a fully developed sunspot in the trailing polarity, and, 3. those that have no sunspot in any polarity. Using SDO/AIA images, we obtain the time frames of the images where the active regions are somewhat steady over a 48 hour time period, without any eruptions or flare-like bursts beyond GOES B-class flares. We select the instances where bright loops are present and choose the nearest SDO/HMI SHARP vector magnetograms in time to perform NLFFF extrapolations using the method of Weigelmann et al. 2004. We also perform differential emission measure calculations over these time-frames of SDO/AIA images to verify the temperature characteristics. We will present the results of these studies for a subset of our active regions, at the 54th SPD meeting.


Tiwari et al., 2017, ApJL, 843, L20

Wiegelmann, T.: 2004, Solar Phys. 219, 87

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