Results 11 to 20 of about 41,225 (263)
Quark star matter in heavy quark stars [PDF]
European Physical Journal C: Particles and Fields, 2021 We study the thermodynamic properties of asymmetric quark matter and large mass quark stars within the confined-isospin-density-dependent-quark-mass model. We find that the quark matter symmetry energy should be very large in order to describe the recent
Peng-Cheng Chu +6 more
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Quark star matter at finite temperature in a quasiparticle model [PDF]
European Physical Journal C: Particles and Fields, 2021 We study the thermodynamic properties of asymmetric quark matter, large mass quark stars (QSs), and proto-quark stars (PQSs) within the quasiparticle model. Considering the effects of temperature within quasiparticle model can significantly influence the
Peng-Cheng Chu +5 more
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The quark strange star in the enlarged Nambu-Jona-Lasinio model [PDF]
, 2002 The strange quark star is investigated within the enlarged SU(3) Nambu-Jona-Lasinio (NJL). The stable quark star exists till maximal configutation with rho_m=3.1, 10^15, g/cm^3 with M_m=1.61, M_Sun and R_m=8.74, km is reached.
Bednarek, I., Manka, R., Przybyla, G.
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Quantum Thermalization Dynamics of Fermi Gases Quenched to the BEC-BCS Crossover. [PDF]
Adv Sci (Weinh)This study, reporting the first experimental realization of interaction quench far faster than the Fermi timescale in fermionic many‐body systems, explores real‐time quantum thermalization dynamics in the BEC‐BCS crossover. It observes prethermal states with distinct lifetimes after quantum quench, uncovers universal prethermal scaling, and observes ...
Yi L, Yu S, Wu M, Deng S, Wu H.
europepmc +2 more sources
Cooling of neutron stars with quark-hadron continuity [PDF]
EPJ Web of Conferences, 2022 Neutron stars are high-density objects formed by the gravitational collapse of massive stars, and the whole star can be likened to a giant nucleus. The interior of a neutron star is considered to contain exotic particles and states which do not appear in
Noda Tsuneo +4 more
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Quark-quark interaction and quark matter in neutron stars [PDF]
Physical Review C, 2022 Hyperon ($Y$) mixing in neutron-star matter brings about a remarkable softening of the equation of state (EoS) and the maximum mass is reduced to a value far less than $2M_{\odot}$. One idea to avoid this "hyperon puzzle in neutron stars" is to assume that the many-body repulsions work universally for every kind of baryons.
Y. Yamamoto, N. Yasutake, Th. A. Rijken
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Neutron Star Mergers and the Quark Matter Equation of State [PDF]
EPJ Web of Conferences, 2022 As neutron stars merge they can approach very high nuclear density. Here, we summarized recent results for the evolution and gravitational wave emission from binary-neutron star mergers using a a variety of nuclear equations of state with and without a ...
Mathews Grant J. +3 more
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The Macro-Physics of the Quark-Nova: Astrophysical Implications
Universe, 2022 A quark-nova is a hypothetical stellar evolution branch where a neutron star converts explosively into a quark star. Here, we discuss the intimate coupling between the micro-physics and macro-physics of the quark-nova and provide a prescription for how ...
Rachid Ouyed
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Bag model and quark star [PDF]
Physical Review D, 2010 In this paper, incorporating the property of the vacuum negative pressure, namely, the bag constant, we presented a new model of the equation of state (EOS) of quark matter at finite chemical potential and zero temperature. By comparing our EOS with Fraga {\it et~al.}'s EOS and SQM1 model, one find that our EOS is softer than Fraga {\it et~al.}'s EOS ...
Hua Li, Luo Xin-Lian, Hong-Shi Zong
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Semi-empirical relation to understand matter properties at neutron star interiors
European Physical Journal C: Particles and Fields, 2022 The occurrence of quark matter at the center of neutron stars is still in debate. This study defines some semi-empirical parameters that try to quantify the presence and the amount of quark matter at star interiors.
Ritam Mallick +2 more
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