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The abundances of 92Nb and 146Sm in the early Solar System are determinedfrom meteoritic analysis and their stellar production is attributed to the pprocess. We investigate if their origin from thermonuclear supernovae derivingfrom the explosion of white dwarfs with mass above the Chandrasekhar limit isin agreement with the abundance of 53Mn, another radionuclide present in theearly Solar System and produced in the same events. A consistent solution for92Nb and 53Mn cannot be found within the current uncertainties and requiresthat the 92Nb/92Mo ratio in the early Solar System is at least 50% lower thanthe current nominal value, which is outside its present error bars. A differentsolution is to invoke another production site for 92Nb, which we find in thealpha-rich freezeout during core-collapse supernovae from massive stars.Whichever scenario we consider, we find that a relatively long time interval ofat least ~10 Myr must have elapsed from when the star-forming region where theSun was born was isolated from the interstellar medium and the birth of theSun. This is in agreement with results obtained from radionuclides heavier thaniron produced by neutron captures and lends further support to the idea thatthe Sun was born in a massive star-forming region together with many thousandsof stellar siblings.

Origin of the p-process radionuclides 92Nb and 146Sm in the early Solar System and inferences on the birth of the Sun