Simulating Hadronic-to-Quark-Matter with Burn-UD: Recent work and astrophysical applications

5th Compact Stars in the QCD Phase Diagram

Welbanks, Luis^1 ; Ouyed, Amir^1 ; Koning, Nico^1 ; Ouyed, Rachid^1

Department of Physics and Astronomy, University of Calgary, 2500 University Drive NW, Calgary

AB

T2N 1N4, Canada^1

关键词: Astrophysical applications;    Burning speed;    Hydrodynamic instabilities;    Neutrino transport;    Neutron density;    Neutron stars;    Supernova explosion;    Time evolutions;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/861/1/012008/pdf
DOI  :  10.1088/1742-6596/861/1/012008

来源: IOP

【 摘 要 】

We present the new developments in Burn-UD, our in-house hydrodynamic combustion code used to model the phase transition of hadronic-to-quark matter. Our two new modules add neutrino transport and the time evolution of a (u, d, s) quark star (QS). Preliminary simulations show that the inclusion of neutrino transport points towards new hydrodynamic instabilities that increase the burning speed. A higher burning speed could elicit the deflagration to detonation of a neutron star (NS) into a QS. We propose that a Quark-Nova (QN: the explosive transition of a NS to a QS) could help us explain the most energetic astronomical events to this day: superluminous supernovae (SLSNe). Our models consider a QN occurring in a massive binary, experiencing two common envelope stages and a QN occurring after the supernova explosion of a Wolf-Rayet (WO) star. Both models have been successful in explaining the double humped light curves of over half a dozen SLSNe. We also introduce SiRop our r-process simulation code and propose that a QN site has the hot temperatures and neutron densities required to make it an ideal site for the r-process.