Abstract: The origin of several proton-rich isotopes in the solar system, most notably $^{92,94}$Mo and $^{96,98}$Ru, remains a long-standing problem in nucleosynthesis. A promising explanation is the $\nu p$-process, which operates in proton-rich, neutrino-driven outflows from the surface of a protoneutron star formed in a core-collapse supernova (CCSN). Years of detailed studies, however, failed to reproduce the observed abundances of various p-nuclei using this process. The efficiency of this mechanism depends on neutrino properties and on the dynamical evolution of the outflow. In this seminar, I will discuss the physical conditions under which the $\nu p$-process successfully reproduces the observed solar abundances of light $p$-nuclides. Computations are performed using refined modeling of the outflow dynamics that self-consistently includes general relativistic effects, which are found to play an important role. In this way, we identify a previously overlooked regime where the $\nu p$-process becomes effective, due to the interplay of different physical effects. Our results suggest that CCSNe from sufficiently massive progenitors can provide a unified explanation for the origin of light $p$-nuclei in the solar system up to $^{102}$Pd.