the fact that this reaction rate is susceptible to the structure of $^{57}$Cu and environs nuclei, including their binding energies. The primary mechanism for producing such nuclei is the rp-process and is believed to be important in the dynamics of the collapsing supermassive stars and x-ray bursts [@Wallace81]. The rp-process is characterized by proton capture reaction rates that are orders of magnitude faster than any other competing process, specially $\beta$-decay rates. The reaction path follows a series of fast (p,$\gamma$)-reactions until further proton capture is inhibited, either by negative proton capture Q-values (proton decay) or small positive proton capture Q-values (photodisintegration). As electrons captures in the stellar pot assist the cooking process and gravity, therefore, it is crucial to know the nuclear structure properties of the doubly magic shell $^{56}$Ni and nuclei in its vicinity. These nuclei drive the electron capture processes in the dense core of heavy mass stars. The beta decay rate calculations require the evaluation of the GT strengths for many levels per nucleus. The pn-QRPA theory gives us the emancipation to use model space as big as $7\, \hbar \omega $ rather than truncated model spaces usually employed in some shell model calculations.

Earlier the half-lives 