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

5th Compact Stars in the QCD Phase Diagram

Hempel, Matthias^1 ; Heinimann, Oliver^1 ; Yudin, Andrey^2 ; Iosilevskiy, Igor^3 ; Liebendörfer, Matthias^1 ; Friedrich-Karl, Thielemann^1

Department of Physics, University of Basel, Klingelbergstr. 82, Basel

CH-4056, Switzerland^1

Institute of Theoretical and Experimental Physics, Moscow

117218, Russia^2

Joint Institute for High Temperatures, Russian Academy of Sciences, Moscow

125412, Russia^3

关键词: Compact stars;    Core collapse supernovae;    Equation of state;    Negative slope;    Neutron stars;    Quark matter;    Temperature phase;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/861/1/012023/pdf
DOI  :  10.1088/1742-6596/861/1/012023

来源: IOP

【 摘 要 】

The QCD phase transition from hadronic to deconfined quark matter is found to be a so-called "entropic" phase transition, characterized, e.g., by a negative slope of the phase transition line in the pressure-temperature phase diagram. In a first part of the present proceedings it is discussed that entropic phase transitions lead to unusual thermal properties of the equation of state (EoS). For example one finds a loss of pressure (a "softening") of the proto-neutron star EoS with increasing entropy. This can lead to a novel, hot third family of compact stars, which exists only in the early proto-neutron star phase. Such a hot third family can trigger explosions of core-collapse supernovae. However, so far this special explosion mechanism was found to be working only for EoSs which are not compatible with the 2 Moconstraint for the neutron star maximum mass. In a second part of the proceeding it is discussed which quark matter parameters could be favorable for this explosion mechanism, and have sufficiently high maximum masses at the same time.