are commonly known as GT transitions. These transitions are ideal probe to test nuclear structure and play preeminent role in the nucleosynthetic origin of the elements in the late phases of the stellar life. When the stellar matter is degenerate then the phase space for the electron in beta decay is Pauli blocked and electron captures become dominant in the stellar core producing neutrinos which escape from the surface of the star and takes away the core energy and entropy as well. These electron capture rates and $\beta^{+}$ decay rates are very sensitive to the distribution of the $GT_{+ }$ strength which is responsible for changing a proton into a neutron (the plus sign is for the isospin raising operator ($t_{+}$), present in the GT matrix elements, which converts a proton into a neutron). The authors in [@Wanajo06; @Kitaura06] took the accurate neutrino transport into account in their hydrodynamic studies of core-collapse supernovae and showed that the bulk of the neutrino-heated ejecta is proton-rich during the early phase $(\leq1 s)$. Their studies also provided that it is likely possible that the neutrino-induced rp-process takes place in all core-collapse supernovae and other astrophysical sites such as collapsar jets or disk winds 