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Gamow-Teller (GT) transitions play an important and consequential role inmany astrophysical phenomena. These include, but are not limited to, electronand positron capture rates which determine the fate of massive stars and playan intricate role in the dynamics of core collapse. These $GT_{\pm}$transitions rates are the significant inputs in the description of supernovaexplosions. $GT_{\pm}$ strength function values are sensitive to the $^{56}Ni$core excitation in the middle \textit{pf}-shell region and to the size of themodel space as well. We used the pn-QRPA theory for extracting the GT strengthfor ground and excited states of $^{56}Ni$. We then used these GT strengthdistributions to calculate the electron \textit{and} positron capture rateswhich show differences with the earlier calculations. One curious finding ofthis paper is our enhanced electron capture rates on $^{56}Ni$ at presupernovatemperatures. These differences need to be taken into account for the modelingof the early stages of Type II supernova evolution.

Gamow-Teller (GT$\pm$) strength distributions of $^{56}Ni$ for ground and excited states