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Abstract

The origin of certain proton-rich nuclides (“p-nuclei”) such as Molybdenum-92,94, Ruthenium-96,98, and Niobium-92 remains an open problem in astrophysics. These nuclei are not produced by the standard neutron-capture processes responsible for most elements heavier than iron, and their solar abundances challenge existing models. Core-collapse supernovae offer an alternative pathway through the \nu-p-process, where neutrino interactions enable their synthesis. However, neutrino flavor conversions remain a major uncertainty in modeling these explosions. In this talk, I will discuss how neutrino oscillations can be modeled in supernovae and how they may provide a robust mechanism to produce these p-nuclei within seconds after the explosion.