scholarly journals Quantum Nucleation of Two-Flavor Quark Matter in Neutron Stars

1997 ◽  
Vol 98 (1) ◽  
pp. 277-282 ◽  
Author(s):  
K. Iida ◽  
K. Sato
Keyword(s):  
Neutron Stars ◽  
Quark Matter ◽  
Quantum Nucleation

Quark matter in neutron stars

2004 ◽  
Vol 19 (S1) ◽  
pp. 189-196
Author(s):  
Marcello Baldo
Keyword(s):  
Neutron Stars ◽  
Quark Matter

scholarly journals Converting neutron stars into strange stars: Instanton model

2014 ◽  
Vol 23 (09) ◽  
pp. 1450078
Author(s):  
Victor Ts. Gurovich ◽  
Leonid G. Fel
Keyword(s):  
Field Theory ◽  
Quantum Field Theory ◽  
Detonation Wave ◽  
Neutron Stars ◽  
Quark Matter ◽  
Quantum Fluctuation ◽  
The Self ◽  
Quantum Field ◽  
Spherical Detonation ◽  
Self Similar

We calculate the quasiclassical probability to emerge the quantum fluctuation which gives rise to the quark-matter drop with interface propagating as the self-similar spherical detonation wave (DN) in the ambient nuclear matter. For this purpose, we make use of instanton method which is known in the quantum field theory.

Phase transition to quark matter in neutron stars

1981 ◽  
Vol 98 (1-2) ◽  
pp. 140-144 ◽  
Author(s):  
Enrique Alvarez
Keyword(s):  
Phase Transition ◽  
Neutron Stars ◽  
Quark Matter

Quark Clustering and Chiral Symmetry Breaking in Nuclear Matter

2003 ◽  
Vol 18 (32) ◽  
pp. 2255-2264 ◽  
Author(s):  
O. A. Battistel ◽  
G. Krein
Keyword(s):  
Symmetry Breaking ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Chiral Symmetry ◽  
Quark Matter ◽  
Traditional Approach ◽  
Chiral Symmetry Breaking ◽  
Quark Condensate ◽  
Baryon Density ◽  
Hadronic Matter

Chiral symmetry breaking at finite baryon density is usually discussed in the context of quark matter, i.e. a system of deconfined quarks. Many systems like stable nuclei and neutron stars however have quarks confined within nucleons. In this paper we construct a Fermi sea of three-quark nucleon clusters and investigate the change of the quark condensate as a function of baryon density. We study the effect of quark clustering on the in-medium quark condensate and compare results with the traditional approach of modeling hadronic matter in terms of a Fermi sea of deconfined quarks.

Neutron stars' quark matter not so strange

Science ◽  
2018 ◽  
Vol 360 (6390) ◽  
pp. 697-697 ◽  
Author(s):  
Adrian Cho
Keyword(s):  
Neutron Stars ◽  
Quark Matter

scholarly journals Evidence for quark-matter cores in massive neutron stars

2020 ◽  
Vol 16 (9) ◽  
pp. 907-910 ◽  
Author(s):  
Eemeli Annala ◽  
Tyler Gorda ◽  
Aleksi Kurkela ◽  
Joonas Nättilä ◽  
Aleksi Vuorinen
Keyword(s):  
Neutron Stars ◽  
Quark Matter

Hyperonic stars within the Bogoliubov quark meson model for nuclear matter

2019 ◽  
Vol 28 (05) ◽  
pp. 1950034
Author(s):  
Prafulla K. Panda ◽  
Constança Providência ◽  
Steven A. Moszkowski ◽  
Henrik Bohr ◽  
João da Providência
Keyword(s):  
Neutron Stars ◽  
Nuclear Matter ◽  
Quark Matter ◽  
Present Model ◽  
Massive Stars ◽  
Symmetric Nuclear Matter ◽  
The Core ◽  
Meson Coupling

We generalize the Bogoliubov quark-meson coupling (QMC) model to also include hyperons. The hyperon-[Formula: see text]-meson couplings are fixed by the model and the hyperon-[Formula: see text]-meson couplings are fitted to the hyperon potentials in symmetric nuclear matter. The present model predicts neutron stars with masses above 2[Formula: see text] and the radius of a 1.4[Formula: see text] star [Formula: see text]14[Formula: see text]km. In the most massive stars, bags overlap at the core of the star, and this may be interpreted as a transition to deconfined quark matter.

FINITE TEMPERATURE EQUATIONS OF STATE FOR MIXED STARS

2004 ◽  
Vol 13 (07) ◽  
pp. 1249-1253
Author(s):  
DÉBORA P. MENEZES ◽  
C. PROVIDÊNCIA
Keyword(s):  
Field Theory ◽  
Neutron Stars ◽  
Quark Matter ◽  
Finite Temperature ◽  
Equations Of State ◽  
Mean Field Theory ◽  
Mean Field ◽  
Relativistic Mean Field Theory ◽  
Relativistic Mean Field

We investigate the properties of mixed stars formed by hadronic and quark matter in β-equilibrium described by appropriate equations of state (EOS) in the framework of relativistic mean-field theory. The calculations were performed for T=0 and for finite temperatures and also for fixed entropies with and without neutrino trapping in order to describe neutron and proto-neutron stars. The star properties are discussed. Maximum allowed masses for proto-neutron stars are much larger when neutrino trapping is imposed.

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