5th Compact Stars in the QCD Phase Diagram | |
Simulating Hadronic-to-Quark-Matter with Burn-UD: Recent work and astrophysical applications | |
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 |
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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.
【 预 览 】
Files | Size | Format | View |
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Simulating Hadronic-to-Quark-Matter with Burn-UD: Recent work and astrophysical applications | 245KB | download |