scholarly journals Bayesian inference of the dense-matter equation of state encapsulating a first-order hadron-quark phase transition from observables of canonical neutron stars

2021 ◽  
Vol 103 (3) ◽  
Author(s):  
Wen-Jie Xie ◽  
Bao-An Li
Keyword(s):  
Phase Transition ◽  
Bayesian Inference ◽  
Equation Of State ◽  
Neutron Stars ◽  
Dense Matter ◽  
First Order ◽  
Quark Phase

scholarly journals Does a hadron-quark phase transition in dense matter preclude the existence of massive neutron stars?

2012 ◽  
Vol 8 (S291) ◽  
pp. 356-358 ◽  
Author(s):  
N. Chamel ◽  
A. F. Fantina ◽  
J. M. Pearson ◽  
S. Goriely
Keyword(s):  
Phase Transition ◽  
Equation Of State ◽  
Neutron Stars ◽  
Nuclear Energy ◽  
Dense Matter ◽  
Density Functionals ◽  
Nuclear Mass ◽  
Neutron Star Mass ◽  
The Impact ◽  
Quark Phase

AbstractWe study the impact of a hadron-quark phase transition on the maximum neutron-star mass. The hadronic part of the equation of state relies on the most up-to-date Skyrme nuclear energy density functionals, fitted to essentially all experimental nuclear mass data and constrained to reproduce the properties of infinite nuclear matter as obtained from microscopic calculations using realistic forces. We show that the softening of the dense matter equation of state due to the phase transition is not necessarily incompatible with the existence of massive neutron stars like PSR J1614–2230.

scholarly journals Phase transitions in neutron stars

2018 ◽  
Vol 27 (11) ◽  
pp. 1830008 ◽  
Author(s):  
V. Dexheimer ◽  
L. T. T. Soethe ◽  
J. Roark ◽  
R. O. Gomes ◽  
S. O. Kepler ◽  
...  
Keyword(s):  
Phase Transition ◽  
Phase Transitions ◽  
Equation Of State ◽  
Neutron Stars ◽  
Order Phase Transition ◽  
Dense Matter ◽  
First Order ◽  
The Core ◽  
First Order Phase Transition ◽  
First Order Phase

In this paper, we review the most common descriptions for the first-order phase transition to deconfined quark matter in the core of neutron stars. We also present a new description of these phase transitions in the core of proto-neutron stars, in which more constraints are enforced so as to include trapped neutrinos. Finally, we calculate the emission of gravitational waves associated with deconfinement phase transitions, discuss the possibility of their detection, and how this would provide information about the equation of state of dense matter.

ON THE CONFINED–DECONFINED PHASE TRANSITION IN NUCLEAR MATTER AND NEUTRON STARS

2010 ◽  
Vol 19 (08n10) ◽  
pp. 1563-1568 ◽  
Author(s):  
L. N. BURIGO ◽  
B. E. J. BODMANN ◽  
R. B. JACOBSEN ◽  
C. A. Z. VASCONCELLOS ◽  
F. FERNÁNDEZ
Keyword(s):  
Phase Transition ◽  
Neutron Stars ◽  
Baryon Number ◽  
Local Conservation ◽  
Independent Components ◽  
First Order ◽  
Mit Bag Model ◽  
Effective Theories ◽  
Quark Phase ◽  
Hadronic Model

In this work we focus our study on the transition from hadron to deconfined quark matter, and we shall assume that the phase transition is first-order with two independent components, which are related to the local conservation of baryon number and the global conservation of electric charge. Relativistic effective theories are employed to describe the hadron and quark phase. Two different hadronic models are adopted: an adjustable model and the well known Boguta–Bodmer model. Deconfined phase is described employing the MIT bag model. Previous studies showed that the choice of the hadronic model as well as its parameters (including nucleon effective mass and hyperonic coupling schemes) have influence on phase transition properties. Our aim is to analyze if such results on phase transition play an important role on the modeling of neutron stars. To carry out such analysis, the Tolman–Oppenheimer–Volkoff equations are employed to determine the maximum mass for each combination of hadronic model and parameters.

HADRON-QUARK PHASE TRANSITION AND ANTIKAON CONDENSATION IN NEUTRON STARS

2008 ◽  
Vol 23 (27n30) ◽  
pp. 2481-2484
Author(s):  
H. SHEN ◽  
F. YANG ◽  
P. YUE
Keyword(s):  
Field Theory ◽  
Phase Transition ◽  
Equation Of State ◽  
Neutron Stars ◽  
Mean Field Theory ◽  
Mean Field ◽  
Maximum Mass ◽  
Relativistic Mean Field ◽  
The Core ◽  
Quark Phase

We study the hadron-quark phase transition and antikaon condensation which may occur in the core of massive neutron stars. The relativistic mean field theory is used to describe the hadronic phase, while the Nambu-Jona-Lasinio model is adopted for the quark phase. We find that the hadron-quark phase transition is very sensitive to the models used. The appearance of deconfined quark matter and antikaon condensation can soften the equation of state at high density and lower the maximum mass of neutron stars.

scholarly journals Equations of State in Stellar Structure and Evolution

1994 ◽  
Vol 147 ◽  
pp. 1-15
Author(s):  
H. M. Van Horn
Keyword(s):  
Phase Transition ◽  
Equation Of State ◽  
White Dwarfs ◽  
Equations Of State ◽  
Dense Matter ◽  
Reaction Rates ◽  
Stellar Structure ◽  
First Order ◽  
First Order Phase Transition ◽  
First Order Phase

AbstractIn this paper I summarize some of the recent advances in studies of dense matter. Research on phase separation in the binary ionic mixtures (BIMs) that constitute the matter in white dwarfs has been motivated by the need to obtain accurate estimates for the ages of the faintest white dwarfs and thus of the disk of our Galaxy. Substantial age increases appear possible, but it is not yet clear whether such large increases occur in real white dwarfs. A second advance is the prediction, based on state-of-the-art physical calculations, that ionization of H at low temperatures and increasing densities may occur via a first-order “plasma phase transition” (PPT). Astrophysical consequences of this result are still being explored in an effort to test this prediction. Related to these equation-of-state calculations are calculations of the enhancement of nuclear reaction rates at high densities. New thermonuclear rates have been computed for C+C reactions in BIMs, although there is currently some controversy about results at the highest densities. New pycnonuclear reaction rates have also been calculated for BIMs, and it has been suggested that He-burning at T = 0 may occur through a first-order phase transition. Finally, calculations of the equation of state of matter in strong magnetic fields and of radiative opacities at high densities have undergone very recent and substantial improvements, which are just beginning to be utilized in astrophysical calculations.

scholarly journals Twin stars: probe of phase transition from hadronic to quark matter

2021 ◽  
Vol 252 ◽  
pp. 06001
Author(s):  
Themistoklis Deloudis ◽  
Polychronis Koliogiannis ◽  
Charalampos Moustakidis
Keyword(s):  
Phase Transition ◽  
Neutron Stars ◽  
Quark Matter ◽  
Compact Stars ◽  
Stable Configuration ◽  
First Order ◽  
Maxwell Construction ◽  
First Order Transition ◽  
Hybrid Stars ◽  
Quark Phase

In agreement with the gravitational-wave events which are constantly increasing, new aspects of the internal structure of compact stars have come to light. A scenario in which a first order transition takes place inside these stars is of particular interest as it can lead, under conditions, to a third gravitationally stable branch (besides white dwarfs and neutron stars). This is known as the twin star scenario. The new branch yields stars with the same mass as normal compact stars but quite different radii. In the current work, we focus on hybrid stars undergone a hadron to quark phase transition near their core and how this new stable configuration arises. Emphasis is to be given especially in the aspects of the phase transition and its parametrization in two different ways, namely with Maxwell construction and with Gibbs construction. Qualitative findings of mass-radius relations of these stars will also be presented.

scholarly journals INVESTIGATION OF THE EXISTENCE OF HYBRID STARS USING NAMBU–JONA–LASINIO MODELS

2010 ◽  
Vol 19 (08n10) ◽  
pp. 1521-1524 ◽  
Author(s):  
J. G. COELHO ◽  
C. H. LENZI ◽  
M. MALHEIRO ◽  
R. M. MARINHO ◽  
M. FIOLHAIS
Keyword(s):  
Phase Transition ◽  
Equation Of State ◽  
Neutron Stars ◽  
Quark Matter ◽  
Chemical Potential ◽  
Compact Stars ◽  
Vector Coupling ◽  
Njl Model ◽  
Hybrid Stars ◽  
Quark Phase

We investigate the hadron-quark phase transition inside neutron stars and obtain mass–radius relations for hybrid stars. The equation of state for the quark phase using the standard NJL model is too soft, leading to an unstable star and suggesting a modification of the NJL model by introducing a momentum cutoff dependent on the chemical potential. However, even in this approach, the instability remains. In order to remedy the instability we suggest the introduction of a vector coupling in the NJL model, which makes the EoS stiffer, reducing the instability. We conclude that the possible existence of quark matter inside the stars require high densities, leading to very compact stars.

Sign in / Sign up

Export Citation Format

Share Document