scholarly journals Combustion of Hadrons to Strange Quark Matter Inside a Neutron Star

2017 ◽  
Vol 45 ◽  
pp. 1760028
Author(s):  
Jhon Andersson Rosero ◽  
Ernesto Kemp
Keyword(s):  
Phase Transition ◽  
Quark Matter ◽  
Strange Quark ◽  
Boltzmann Transport Equation ◽  
Strange Quark Matter ◽  
Strong Interactions ◽  
Boltzmann Transport ◽  
Coupling Constant ◽  
Interaction Processes ◽  
Perturbative Regime

We have studied the phase transition from hadronic to quark matter inside neutron stars, we calculate the rate and emissivity for all the relevant weak interaction processes and solve the Boltzmann transport equation, considering the effect of strong interactions in the perturbative regime to the order of QCD coupling constant [Formula: see text]. We find that the neutrino and antineutrino emissivity is around of 10[Formula: see text] erg.

scholarly journals Color flavor locked phase transition in strange quark matter

2007 ◽  
Vol 37 (1a) ◽  
pp. 20-22 ◽  
Author(s):  
Milva Orsaria ◽  
H. Rodrigues ◽  
S. B. Duarte
Keyword(s):  
Phase Transition ◽  
Quark Matter ◽  
Strange Quark ◽  
Strange Quark Matter

scholarly journals Simulating Binary Neutron Stars with Hybrid Equation of States: Gravitational Waves, Electromagnetic Signatures and Challenges for Numerical Relativity

Particles ◽  
2019 ◽  
Vol 2 (3) ◽  
pp. 365-384 ◽  
Author(s):  
Henrique Gieg ◽  
Tim Dietrich ◽  
Maximiliano Ujevic
Keyword(s):  
Phase Transition ◽  
Equation Of State ◽  
Neutron Stars ◽  
Gravitational Wave ◽  
Quark Matter ◽  
Strange Quark ◽  
Numerical Relativity ◽  
Strange Quark Matter ◽  
Strong Phase ◽  
Equation Of States

The gravitational wave and electromagnetic signatures connected to the merger of two neutron stars allow us to test the nature of matter at supranuclear densities. Since the Equation of State governing the interior of neutron stars is only loosely constrained, there is even the possibility that strange quark matter exists inside the core of neutron stars. We investigate how strange quark matter cores affect the binary neutron star coalescence by performing numerical relativity simulations. Interestingly, the strong phase transition can cause a reduction of the convergence order of the numerical schemes to first order if the numerical resolution is not high enough. Therefore, an additional challenge is added in producing high-quality gravitational wave templates for Equation of States with a strong phase transition. Focusing on one particular configuration of an equal mass configuration consistent with GW170817, we compute and discuss the associated gravitational wave signal and some of the electromagnetic counterparts connected to the merger of the two stars. We find that existing waveform approximants employed for the analysis of GW170817 allow describing this kind of systems within the numerical uncertainties, which, however, are several times larger than for pure hadronic Equation of States, which means that even higher resolutions have been employed for an accurate gravitational wave model comparison. We also show that for the chosen Equation of State, quasi-universal relations describing the gravitational wave emission after the moment of merger seem to hold and that the electromagnetic signatures connected to our chosen setup would not be bright enough to explain the kilonova associated to GW170817.

PHASE TRANSITION IN STRANGE QUARK MATTER WITH DENSITY DEPENDENT QUARK MASS

2007 ◽  
Vol 16 (02n03) ◽  
pp. 291-295 ◽  
Author(s):  
M. ORSARIA ◽  
H. RODRIGUES ◽  
S. B. DUARTE
Keyword(s):  
Phase Transition ◽  
Quark Matter ◽  
Strange Quark ◽  
Baryon Number ◽  
Strange Quark Matter ◽  
Zero Temperature ◽  
Number Density ◽  
Quark Masses ◽  
Dense System ◽  
Color Superconductor

We investigate the color superconducting phase transition in strange quark matter at zero temperature considering the density dependence of quark masses. At high densities, it is well known that cold quark matter is a color superconductor with favorable phase being the color flavor locked (CFL). We analyze the phase transition between the initially strange quark matter (SQM) and the CFL phases. The quark masses are parametrized with the baryon number density nB in the dense system.

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