high temperatures where nuclear statistical equilibrium is valid. According to studies by authors in Ref. [@Schatz98] the peak conditions for rp-process are in the vicinity of T = (1–3) GK and $\rho = (10^{6}-10^{7}$) gcm$^{-3}$. The current analysis shows that the electron capture and positron decay rates of $^{57}$Zn contribute roughly equally to the total weak rates at peak rp-process conditions (with the positron decay rates bigger roughly by a factor of 6–7). At still higher temperatures and densities the electron capture on $^{57}$Zn dominates . As a result both $\beta^{+}$ and electron capture stellar rates on $^{57}$Zn are being presented in this paper.

Section 2 describes the theoretical formalism of pn-QRPA calculation. Section 3 discusses the pn-QRPA calculated GT strength functions and its comparison with measurements and previous calculation. The calculated weak rates are presented in Section 4. Here we also compare our results with the pioneering calculation of Fuller and collaborators [@Fuller82]. We finally conclude our findings in Section 5.

Model Description
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The nuclei involved in the stellar interior have finite probability of occupation of excited states and the state by state evaluation of the GT strength distribution from these excited states is a formidable task. The 