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Here, we study the temperature structure of flaring and non-flaring coronalloops, using extracted loops from images taken in six extreme ultraviolet (EUV)channels recorded by Atmospheric Imaging Assembly (AIA)/ Solar DynamicObservatory (SDO). We use data for loops of X2.1-class-flaring active region(AR11283) during 22:10UT till 23:00UT, on 2011, September 6; and non-flaringactive region (AR12194) during 08:00:00UT till 09:00:00UT on 2014, October 26.By using spatially-synthesized Gaussian DEM forward-fitting method, wecalculate the peak temperatures for each strip of the loops. We apply theLomb-Scargle method to compute the oscillations periods for the temperatureseries of each strip. The periods of the temperature oscillations for theflaring loops are ranged from 7 min to 28.4 min. These temperature oscillationsshow very close behavior to the slow-mode oscillation. We observe that thetemperature oscillations in the flaring loops are started at least around 10minutes before the transverse oscillations and continue for a long timeduration even after the transverse oscillations are ended. The temperatureamplitudes are increased at the flaring time (during 20 min) in the flaringloops. The periods of the temperatures obtained for the non-flaring loops areranged from 8.5 min to 30 min, but their significances are less (below 0.5) incomparison with the flaring ones (near to one). Hence the detected temperatureperiods for the non-flaring loops' strips are less probable in comparison withthe flaring ones, and maybe they are just fluctuations.  Based on our confined observations, it seems that the flaring loops' periodsshow more diversity and their temperatures have wider ranges of variation thanthe non-flaring ones. More accurate commentary in this respect requires moreextensive statistical research and broader observations.

Temperature Analysis of Flaring (AR11283) and non-Flaring (AR12194) Coronal Loops