has to rely on theoretical models for the calculation of GT strength distributions in high excitation energies region as well as for parent excited states. Within the $Q$ window of the reaction, we extracted a total GT strength of 15.23 and the KB3G calculation amount it to be 8.63. The pn-QRPA results include a quenching factor of 0.8 as usually employed for the *pf*-shell nuclei. The luxurious $7\, \hbar \omega $ model space of the pn-QRPA facilitates one to extract the state by state evaluation of the these GT strength for higher excited states as well without assuming the Brink’s hypothesis and model space truncation as usually employed in the shell model calculations. The truncation level, i.e, the number of nucleons which are to be excited from the $f_{7/2}$ orbital to the rest of the *pf*-shell, in the KB3G calculation was restricted to 4 nucleons for parent $^{57}$Zn and 5 nucleons for daughter $^{57}$Cu. The pn-QRPA model extracted a bigger total strength as compared to the KB3G interactions employed in the shell model calculation. This certainly affects the calculation of $\beta^{+}$-decay and electron capture rates in the stellar core at high densities. Except at higher temperatures, the double shell closure 