New aspects of the QCD phase transition in proto-neutron stars and core-collapse supernovae

Hempel, Matthias; Heinimann, Oliver; Yudin, A. V.; Iosilevskiy, Igor; Liebendörfer, M.; Thielemann, Friedrich‐Karl

doi:10.1088/1742-6596/861/1/012023

Cited by 2 publications

(1 citation statement)

References 32 publications

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“…Now, in the case of the liquid-gas phase transition (general or nuclear), dP/dT is positive and, thus, correctly implies that S B,G > S B,L . In the case of the deconfinement phase transition in heavy-ion matter [4,60] and neutron star matter [61], dP/dT was shown to be instead negative. This then implies that S B,Q > S B,H , which is quite natural as the quarks contain extra color degrees of freedom.…”

Section: Resultsmentioning

confidence: 97%

Deconfinement phase transition in proto-neutron-star matter

Roark

Dexheimer

2018

Phys. Rev. C

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In this work, we study in detail the deconfinement phase transition that takes place in hot/dense nuclear matter in the context of neutron stars and proto-neutron stars (in which lepton fraction is fixed). The possibility of different mixtures of phases with different locally and globally conserved quantities is considered in each case. For this purpose, the Chiral Mean Field (CMF) model, an effective relativistic model that includes self-consistent chiral symmetry restoration and deconfinement to quark matter, is employed. Finally, we compare our results with blue results provided by PQCD for different temperatures and conditions.

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Section: Resultsmentioning

confidence: 97%

Deconfinement phase transition in proto-neutron-star matter

Roark

Dexheimer

2018

Phys. Rev. C

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The role of the hadron-quark phase transition in core-collapse supernovae

Jakobus

Müller

Heger

et al. 2022

Monthly Notices of the Royal Astronomical Society

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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 $14\texttt {-}100\, \text{M}_\odot$. We find explosions only for two low-compactness models (14M⊙ and 16 M⊙) with the DD2F_SF EoS, both with low explosion energies of $\mathord {\sim }10^{50}\, \mathrm{erg}$. 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 90Zr for the 14 M⊙ zero-metallicity model and 94Zr for the 16 M⊙ 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 4kB/baryon and may have a distinctive gravitational wave signature, also for a second-order phase transition.

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New aspects of the QCD phase transition in proto-neutron stars and core-collapse supernovae

Cited by 2 publications

References 32 publications

Deconfinement phase transition in proto-neutron-star matter

Deconfinement phase transition in proto-neutron-star matter

The role of the hadron-quark phase transition in core-collapse supernovae

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