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Soon after the collapse of a massive star, very high densities and temperatures can be achieved. In particular, such conditions may allow for a phase transition from nuclear matter to quark matter. Assuming this phase transition to be of first order, the simplest mechanism for phase conversion is the nucleation of bubbles of the quark phase inside the uniform nuclear matter phase. In this work, we compare the nucleation time scales with the typical time scale of the early post-bounce phase in a supernova explosion. We find that nucleation is a feasible mechanism for phase conversion in this scenario only if the surface tension between the nuclear and the quark phases has a relatively small value.

Thermal Nucleation of Quark Matter in a Lepton-Rich Environment