  Here, we study the temperature structure of flaring and non-flaring coronal
loops, using extracted loops from images taken in six extreme ultraviolet (EUV)
channels recorded by Atmospheric Imaging Assembly (AIA)/ Solar Dynamic
Observatory (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-flaring
active region (AR12194) during 08:00:00UT till 09:00:00UT on 2014, October 26.
By using spatially-synthesized Gaussian DEM forward-fitting method, we
calculate the peak temperatures for each strip of the loops. We apply the
Lomb-Scargle method to compute the oscillations periods for the temperature
series of each strip. The periods of the temperature oscillations for the
flaring loops are ranged from 7 min to 28.4 min. These temperature oscillations
show very close behavior to the slow-mode oscillation. We observe that the
temperature oscillations in the flaring loops are started at least around 10
minutes before the transverse oscillations and continue for a long time
duration even after the transverse oscillations are ended. The temperature
amplitudes are increased at the flaring time (during 20 min) in the flaring
loops. The periods of the temperatures obtained for the non-flaring loops are
ranged from 8.5 min to 30 min, but their significances are less (below 0.5) in
comparison with the flaring ones (near to one). Hence the detected temperature
periods for the non-flaring loops' strips are less probable in comparison with
the flaring ones, and maybe they are just fluctuations.
  Based on our confined observations, it seems that the flaring loops' periods
show more diversity and their temperatures have wider ranges of variation than
the non-flaring ones. More accurate commentary in this respect requires more
extensive statistical research and broader observations.
