My work includes the evolution of the Flare and the active region AR11748 where
the X1.2 class
are is observed on May 15, 2013 with the magnetic complexity
.
The active region was spread in the area of 310 km2 in the North-Eastern limb
of the Sun. I have analyzed the region and
are with different wavelength data
sets to nd its evolutionary behavior. Flare shows the two ribbon structure and I
also found that stationary brightening propagates along the southern ribbon. On
the contrary, I found the emerging material from the same region was the driver
of the instability. I did not nd the any lament associated with the
are. For
the morphological evolution of the active region, I have used SDO data and I have
used SDO/HMI magnetograms and the velocity Dopplergrams for the photospheric
magnetic parameters. From this study, I conclude that
are occurred in the lower
corona and the coronal loops moved upward which gives the signature of the magnetic
reconnection beneath the uprising loops.