Gamma-ray bursts generated from phase transition of neutron stars to quark stars

2017 ◽  
Vol 32 (04) ◽  
pp. 1750027 ◽  
Author(s):  
Xiao-Yu Shu ◽  
Yong-Feng Huang ◽  
Hong-Shi Zong
Keyword(s):  
Phase Transition ◽  
Neutron Stars ◽  
Gamma Ray ◽  
Mean Field ◽  
Gamma Ray Bursts ◽  
Compact Stars ◽  
Particle Model ◽  
Relativistic Mean Field ◽  
Quark Stars ◽  
Quark Phase

The evolution of compact stars is believed to be able to produce various violent phenomena in our universe. In this paper, we discuss the possibility that gamma-ray bursts (GRBs) might result from the phase transition of a neutron star to a quark star and calculate the energy released from the conversion. In our study, we utilize the relativistic mean field (RMF) theory to describe the hadronic phase of neutron stars, while an improved quasi-particle model is adopted to describe the quark phase of quark stars. With quark matter equation-of-state (EOS) more reliable than models used before, it is found that the energy released is of the order of 10[Formula: see text] erg, which confirms the validity of the phase transition model.

Conversion of neutron stars to 2 + 1 flavor Nambu–Jona-Lasinio quark stars as a mechanism for gamma-ray bursts

2017 ◽  
Vol 32 (37) ◽  
pp. 1750209
Author(s):  
Xiao-Yu Shu ◽  
Yong-Feng Huang ◽  
Hong-Shi Zong
Keyword(s):  
Phase Transition ◽  
Gamma Ray ◽  
Chemical Potential ◽  
Proper Time ◽  
Mean Field ◽  
Gamma Ray Bursts ◽  
Compact Stars ◽  
Relativistic Mean Field ◽  
Quark Stars ◽  
Njl Model

The phase transition from a neutron star to a quark star and its relation to gamma-ray bursts are investigated. A new model: the 2 + 1 flavor Nambu–Jona-Lasinio (NJL) model with the method of proper-time regularization (PTR) is utilized for the quark phase; while the Relativistic Mean Field (RMF) theory is used for the hadronic phase. The process of phase transition is studied by considering the chemical potential, paying special attention to the phase transition point and the emergence of strange quark matter. Characteristics of compact stars are illustrated, and the energy release during the phase transition is found to be [Formula: see text] erg.

scholarly journals ENERGY RELEASE ASSOCIATED WITH QUARK PHASE TRANSITION IN NEUTRON STARS: COMPARATIVE ANALYSIS OF MAXWELL AND GLENDENNING SCENARIOS

2012 ◽  
Vol 18 ◽  
pp. 1-9
Author(s):  
ANI ALAVERDYAN ◽  
GRIGOR ALAVERDYAN ◽  
SHUSHAN MELIKYAN
Keyword(s):  
Phase Transition ◽  
Mean Field ◽  
Effective Field ◽  
Compact Stars ◽  
Relativistic Mean Field ◽  
Hadron Phase ◽  
First Order Phase Transition ◽  
Deconfinement Phase Transition ◽  
The One ◽  
Quark Phase

We study the compact stars internal structure and observable characteristics alterations due to the quark deconfinement phase transition. To proceed with, we investigate the properties of isospin- asymmetric nuclear matter in the improved relativistic mean-field (RMF) theory, including a scalar-isovector δ-meson effective field. In order to describe the quark phase, we use the improved version of the MIT bag model, in which the interactions between u, d and s quarks inside the bag are taken into account in the one-gluon exchange approximation. We compute the amount of energy released by the corequake for both cases of deconfinement phase transition scenarios, corresponding to the Maxwellian type ordinary first-order phase transition and the phase transition with formation of a mixed quark-hadron phase (Glendenning scenario).

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 Constraining bag constant for hybrid neutron stars

2020 ◽  
Vol 29 (07) ◽  
pp. 2050044
Author(s):  
Ishfaq A. Rather ◽  
Ankit Kumar ◽  
H. C. Das ◽  
M. Imran ◽  
A. A. Usmani ◽  
...  
Keyword(s):  
Neutron Stars ◽  
Mean Field ◽  
Effective Field ◽  
Mean Field Model ◽  
Relativistic Mean Field ◽  
Hadron Phase ◽  
Neutron Star Mass ◽  
Mit Bag Model ◽  
Quark Phase ◽  
Bag Constant

We study the star matter properties for Hybrid equation of state (EoS) by varying the bag constant. We use the effective field theory motivated relativistic mean field model (E-RMF) for hadron phase with recently reported FSUGarnet, G3 and IOPB-I parameter sets. The results of NL3 and NL3[Formula: see text] sets are also shown for comparison. The simple MIT bag model is applied for the quark phase to construct the hybrid EoS. The hybrid neutron star mass and radius are calculated by varying with [Formula: see text] to constrain the [Formula: see text] values. It is found that [Formula: see text]–160[Formula: see text]MeV is suitable for explaining the quark matter in neutron stars.

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.

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 A Bayesian Analysis on Neutron Stars within Relativistic Mean Field Models

Particles ◽  
2020 ◽  
Vol 3 (3) ◽  
pp. 621-629
Author(s):  
Prasanta Char ◽  
Silvia Traversi ◽  
Giuseppe Pagliara
Keyword(s):  
Phase Transition ◽  
Equation Of State ◽  
Bayesian Analysis ◽  
Neutron Stars ◽  
Mean Field ◽  
Chiral Phase ◽  
Relativistic Mean Field ◽  
Mean Field Models ◽  
Adopted Model ◽  
Nuclear Incompressibility

We present a Bayesian analysis on the equation of state of neutron stars based on a class of relativistic mean field models. The priors on the equation of state are related to the properties of nuclear matter at saturation and the posteriors are obtained through the Bayesian procedure by exploiting recent astrophysical constraints on the mass–radius relations of neutron stars. We find indications of a tension (within the adopted model) between the prior on the nuclear incompressibility and its posterior which in turn seems to suggest a possible phase transition at about twice saturation density to a phase where the nucleon effective mass is strongly reduced. A possible relation with the chiral phase transition in dense matter is also discussed.

scholarly journals DECONFINEMENT PHASE TRANSITION IN NEUTRON STARS AND δ-MESON FIELD IN RMF THEORY

2010 ◽  
Vol 19 (08n10) ◽  
pp. 1557-1561 ◽  
Author(s):  
A. G. ALAVERDYAN ◽  
G. B. ALAVERDYAN ◽  
A. O. CHILADZE
Keyword(s):  
Phase Transition ◽  
Mean Field ◽  
Exchange Interactions ◽  
Meson Field ◽  
Relativistic Mean Field ◽  
Mit Bag Model ◽  
Deconfinement Phase Transition ◽  
Boundary Characteristics ◽  
Quark Phase ◽  
Phase Transition Boundary

The Maxwell and Glendenning construction scenarios of deconfinement phase transition in neutron star matter are investigated. The hadronic phase is described within the relativistic mean-field (RMF) theory, if the scalar-isovector δ-meson field is also taken into account. The strange quark phase is described in the frame of MIT bag model, including the effect of perturbative one-gluon exchange interactions. The influence of the δ-meson field on the deconfinement phase transition boundary characteristics is discussed.

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