We study the relationship between the physical process of magnetic energy build up and its release as solar flares/ CMEs. We consider the free magnetic field energy in the active region as source of energy build-up in the corona, while gradient and rotation angle of active region as the cause of flares/ CMEs. We undertake the measurement of magnetic field complexity employing HMI/SDO magnetograms to constrain the possible mechanisms providing the energy on one hand and triggering of flares on the other hand. Total 15 super active regions observed during 2010-2015 are selected considering that each has produced minimum 40 flares of ≥C1.0 during its passage on the disk. We measure the magnetic flux to quantifying energy build up, moving from photosphere to corona, while gradient (dH/dz) and rotation angle () of the active region are quantified as the mechanisms for energy release process in the corona. The estimated magnetic flux, gradient and rotation angle are found to vary between 9*1024 -2.8*1026 Mx, 1*10-5–1.25*10-2 gauss/cm and, -87 – +90 degrees respectively. Out of 15 active regions 5 produced proton flares. The GOES X-ray intensity as a function of disk integrated magnetic flux during the passage of the 5 super active regions reveals asymptotic linear relationship. The CME velocity and magnitude protons acceleration is closely associated with the rotation angle of the active region.