The Role of the Hadron-Quark Phase Transition in Core-Collapse Supernovae

Abstract

The hadron-quark phase transition in quantum chromodyanmics has been suggested as an alternative explosion mechanism for core-collapse supernovae. We study the impact of three different hadron-quark equations of state (EoS) with first-order (DD2F\_SF, STOS-B145) and second-order (CMF) phase transitions on supernova dynamics by performing 97 simulations for solar- and zero-metallicity progenitors in the range of $14\text{-}100{\text{M}}_{\odot }$. We find explosions only for two low-compactness models ($14{\text{M}}_{\odot }$ and $16{\text{M}}_{\odot }$) with the DD2F\_SF EoS, both with low explosion energies of $\sim 10^{50}\mathrm{erg}$. These weak explosions are characterised by a neutrino signal with several mini-bursts in the explosion phase due to complex reverse shock dynamics, in addition to the typical second neutrino burst for phase-transition driven explosions. The nucleosynthesis shows significant overproduction of nuclei such as ${}^{90}\mathrm{Zr}$ for the $14{\text{M}}_{\odot }$ zero-metallicity model and ${}^{94}\mathrm{Zr}$ for the $16{\text{M}}_{\odot }$ solar-metallicity model, but the overproduction factors are not large enough to place constraints on the occurrence of such explosions. Several other low-compactness models using the DD2F\_SF EoS and two high-compactness models using the STOS EoS end up as failed explosions and emit a second neutrino burst. For the CMF EoS, the phase transition never leads to a second bounce and explosion. For all three EoS, inverted convection occurs deep in the core of the proto-compact star due to anomalous behaviour of thermodynamic derivatives in the mixed phase, which heats the core to entropies up to $4k_{\text{B}}/\text{baryon}$ and may have a distinctive gravitational wave signature, also for a second-order phase transition.

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