/ Astrophysics


Quark Matter in Core Collapse Supernova Simulations


Fischer, Tobias (Wroclaw U.) ; Klähn, Thomas (Wroclaw U.) ; Sagert, Irina (Indiana U.) ; Hempel, Matthias (Basel U.) ; Blaschke, David (Dubna, JINR)

Published in: Acta Phys.Polon.Supp.
Year: 2014
Vol.: 7    Num./Issue: 1
Page No: 153-161
Pages: 9
Year: 2014 published

Abstract: Any reliable equation of state (EOS) for astrophysical applications faces recently sever constraints, in particular associated with high-precision ob- servations of massive neutron stars. The associated stiffness of the EOS limits the freedom to include additional degrees of freedom at high density, e.g. , hyperons and quarks. For supernova matter, featuring high tempera- tures and large isospin asymmetry, there are only few EOS constraints at high density. We use this freedom and construct a quark–hadron hybrid EOS based on the bag model for strange quark matter. Parameters are selected such that (a) cold compact stars are consistent with observations and (b) quark matter appears close to saturation density. The hadron– quark phase transition is constructed by applying the Gibbs condition. This novel EOS is implemented in core-collapse supernova simulations in spherical symmetry, where we observe only a mild softening of the EOS in the quark–hadron mixed phase. The central protoneutron star (PNS) re- mains stable at all considered times and pure quark matter is never reached. The resulting slow conversion of nuclear matter into strange quark matter due to compression leaves a mild feedback to the neutrino observables as a consequence of the structural reconfiguration of the PNS. Moreover, we give a brief outlook towards more sophisticated quark–matter descriptions, i.e. the Nambu–Jona-Lasinio model and the Dyson–Schwinger formalism.

Total numbers of views: 839
Numbers of unique views: 413
DOI: 10.5506/APhysPolBSupp.7.153
 Record created 2014-06-02, last modified 2014-06-02



Rate this document:

Rate this document:
1
2
3
 
(Not yet reviewed)