scholarly journals Deconfinement Phase Transition Heating and Thermal Evolution of Neutron Stars

2008 ◽  
Author(s):  
Miao Kang ◽  
Nana Pan ◽  
Xiaodong Wang ◽  
Ye-Fei Yuan ◽  
Xiang-Dong Li ◽  
...  
Keyword(s):  
Phase Transition ◽  
Neutron Stars ◽  
Thermal Evolution ◽  
Deconfinement Phase Transition

Antikaon condensation and deconfinement phase transition in neutron stars

2006 ◽  
Vol 73 (5) ◽  
Author(s):  
Jianfa Gu ◽  
Hua Guo ◽  
Xiguo Li ◽  
Yuxin Liu ◽  
Furong Xu
Keyword(s):  
Phase Transition ◽  
Neutron Stars ◽  
Deconfinement Phase Transition

Gamma Ray Bursts from delayed quark-deconfinement phase transition in neutron stars

2002 ◽  
Vol 113 (1-3) ◽  
pp. 268-274 ◽  
Author(s):  
Z. Berezhiani ◽  
I. Bombaci ◽  
A. Drago ◽  
F. Frontera ◽  
A. Lavagno
Keyword(s):  
Phase Transition ◽  
Neutron Stars ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Deconfinement Phase Transition ◽  
Quark Deconfinement

scholarly journals Simplified Thermal Evolution of Proto-Hybrid Stars

2017 ◽  
Vol 45 ◽  
pp. 1760041 ◽  
Author(s):  
Mauro Mariani ◽  
Milva Orsaria ◽  
Héctor Vucetich
Keyword(s):  
Phase Transition ◽  
Neutron Stars ◽  
Thermal Evolution ◽  
Late Phase ◽  
Hadronic Matter ◽  
Maximum Mass ◽  
Hybrid Star ◽  
Star Evolution ◽  
Hybrid Stars ◽  
Quark Phase

We study the possibility of a hadron-quark phase transition in the interior of neutron stars, taking into account different schematic evolutionary stages at finite temperature. Furthermore, we analyze the astrophysical properties of hot and cold hybrid stars, considering the constraint on maximum mass given by the pulsars J1614-2230 and J1614-2230. We obtain cold hybrid stars with maximum masses [Formula: see text] M[Formula: see text]. Our study also suggest that during the proto-hybrid star evolution a late phase transition between hadronic matter and quark matter could occur, in contrast with previous studies of proto-neutron stars.

Joule Heating and the Thermal Evolution of Old Neutron Stars

1998 ◽  
Vol 503 (1) ◽  
pp. 368-373 ◽  
Author(s):  
Juan A. Miralles ◽  
Vadim Urpin ◽  
Denis Konenkov
Keyword(s):  
Neutron Stars ◽  
Joule Heating ◽  
Thermal Evolution

scholarly journals Constraint on phase transition with the multimessenger data of neutron stars

2021 ◽  
Vol 103 (6) ◽  
Author(s):  
Shao-Peng Tang ◽  
Jin-Liang Jiang ◽  
Wei-Hong Gao ◽  
Yi-Zhong Fan ◽  
Da-Ming Wei
Keyword(s):  
Phase Transition ◽  
Neutron Stars

scholarly journals Gluodynamics and deconfinement phase transition under rotation from holography

2021 ◽  
Vol 2021 (7) ◽  
Author(s):  
Xun Chen ◽  
Lin Zhang ◽  
Danning Li ◽  
Defu Hou ◽  
Mei Huang
Keyword(s):  
Phase Transition ◽  
Angular Velocity ◽  
Chemical Potential ◽  
Entropy Density ◽  
Thermodynamic Quantities ◽  
Strongly Coupled ◽  
Trace Anomaly ◽  
Holographic Qcd ◽  
Deconfinement Phase Transition ◽  
Small Chemical

Abstract We investigate rotating effect on deconfinement phase transition in an Einstein-Maxwell-Dilaton (EMD) model in bottom-up holographic QCD approach. By constructing a rotating black hole, which is supposed to be dual to rotating strongly coupled nuclear matter, we investigate the thermodynamic quantities, including entropy density, pressure, energy density, trace anomaly, sound speed and specific heat for both pure gluon system and two-flavor system under rotation. It is shown that those thermodynamic quantities would be enhanced by large angular velocity. Also, we extract the information of phase transition from those thermodynamic quantities, as well as the order parameter of deconfinement phase transition, i.e. the loop operators. It is shown that, in the T − ω plane, for two-flavor case with small chemical potential, the phase transition is always crossover. The transition temperature decreases slowly with angular velocity and chemical potential. For pure gluon system with zero chemical potential, the phase transition is always first order, while at finite chemical potential a critical end point (CEP) will present in the T − ω plane.

scholarly journals Nuclear equation of state and neutron star cooling

2017 ◽  
Vol 26 (04) ◽  
pp. 1750015 ◽  
Author(s):  
Yeunhwan Lim ◽  
Chang Ho Hyun ◽  
Chang-Hwan Lee
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Thermal Evolution ◽  
Observation Data ◽  
Nuclear Equation Of State ◽  
The Core ◽  
Dense Nuclear Matter ◽  
Nuclear Models

In this paper, we investigate the cooling of neutron stars with relativistic and nonrelativistic models of dense nuclear matter. We focus on the effects of uncertainties originated from the nuclear models, the composition of elements in the envelope region, and the formation of superfluidity in the core and the crust of neutron stars. Discovery of [Formula: see text] neutron stars PSR J1614−2230 and PSR J0343[Formula: see text]0432 has triggered the revival of stiff nuclear equation of state at high densities. In the meantime, observation of a neutron star in Cassiopeia A for more than 10 years has provided us with very accurate data for the thermal evolution of neutron stars. Both mass and temperature of neutron stars depend critically on the equation of state of nuclear matter, so we first search for nuclear models that satisfy the constraints from mass and temperature simultaneously within a reasonable range. With selected models, we explore the effects of element composition in the envelope region, and the existence of superfluidity in the core and the crust of neutron stars. Due to uncertainty in the composition of particles in the envelope region, we obtain a range of cooling curves that can cover substantial region of observation data.

scholarly journals Entanglement entropy of AdS5 × S5 with massive flavors

2018 ◽  
Vol 33 (03) ◽  
pp. 1850008
Author(s):  
Sen Hu ◽  
Guozhen Wu
Keyword(s):  
Phase Transition ◽  
Line Segment ◽  
Entanglement Entropy ◽  
Point Of View ◽  
Nucl Phys ◽  
Zero Temperature ◽  
Holographic Entanglement Entropy ◽  
Deconfinement Phase Transition

We consider backreacted [Formula: see text] coupled with [Formula: see text] massive flavors introduced by D7 branes. The backreacted geometry is in the Veneziano limit with fixed [Formula: see text]. By dividing one of the directions into a line segment with length l, we get two subspaces. Then we calculate the entanglement entropy between them. With the method of [I. R. Klebanov, D. Kutasov and A. Murugan, Nucl. Phys. B 796, 274 (2008)], we are able to find the cut-off independent part of the entanglement entropy and finally find that this geometry shows no confinement/deconfinement phase transition at zero temperature from the holographic entanglement entropy point of view similar to the case in pure [Formula: see text].

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