stellar densities (where electron capture rates surpass the $\beta^{+}$ decay rates), $\rho
Y_{e} [gcm^{-3}] \sim 10^{11}$, the FFN rates are in good comparison with the pn-QRPA electron capture rates. At lower densities the pn-QRPA electron capture rates are bigger by a factor 2 (T$_{9} [K]
\sim 1$) to a factor of 3 when T$_{9} [K] = 30$. This enhancement is attributed to the low placement of the GT centroid in the daughter nucleus, $^{57}$Cu, by the pn-QRPA model.

![Comparison of the pn-QRPA and FFN [@Fuller82] electron capture rates on $^{57}$Zn nucleus as a function of temperature for selected densities in stellar matter.[]{data-label="fig5"}](fig.5.eps){width="3.3in" height="4.3in"}

The $\beta^{+}$-decay and electron capture rates on $^{57}$Zn were calculated on a fine grid temperature-density scale suitable for simulation codes and for necessary interpolation purposes. The ASCII files of these rates may be requested from the corresponding author.

Summary
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The GT strength function is an important ingredient in the complex dynamics of presupernova and supernova explosion since these GT transitions partly determine the $\beta^{+}$-decay and electron capture rates in the stellar core. The GT strength distributions in $^{57}$Zn were calculated within the domain of the pn-QRPA theory. The pn-QRPA calculated GT strength showed differences with the 