The maximum mass of a cold neutron star

1975 ◽  
Vol 202 ◽  
pp. 782 ◽  
Author(s):  
J. Rosen ◽  
N. Rosen
Keyword(s):  
Neutron Star ◽  
Cold Neutron ◽  
Maximum Mass

scholarly journals Maximum mass of hybrid star formed via shock induced phase transition in cold neutron stars

2021 ◽  
Author(s):  
Ritam Mallick ◽  
Shailendra Singh ◽  
Rana Nandi
Keyword(s):  
Phase Transition ◽  
Neutron Star ◽  
Cold Neutron ◽  
Local Maximum ◽  
Global Maximum ◽  
Maximum Pressure ◽  
Maximum Mass ◽  
Hybrid Star ◽  
External Energy ◽  
Hybrid Stars

Abstract This article studies the maximum mass limit of the hybrid star formed after the shock-induced phase transition of a cold neutron star. By employing hadronic and quark equation of state that satisfies the current mass bound, we use combustion adiabat conditions to find such a limit. The combustion adiabat condition results in a local or a global maximum pressure at an intermediate density range. The maximum pressure corresponds to a local or global maximum mass for the phase transformed hybrid star. The phase transition is usually exothermic if we have a local maximum mass. The criteria for exothermic or endothermic phase transition depend on whether the quark pressure/energy ratios to nuclear pressure/energy are smaller or greater than 1. We find that exothermic phase transition in a cold neutron star usually results in hybrid stars whose mass is smaller than a parent neutron star. The phase transition is endothermic for a global maximum pressure; thereby, one gets a global maximum mass. Hybrid stars much massive than phase transformed local maximum mass can be formed, provided there is some external energy source during the phase transition process. However, for some cases, even massive hybrid stars can form with exothermic phase transition for equations of state having global maximum pressure.

scholarly journals Astrophysical implications of neutron star inspiral and coalescence

2020 ◽  
Vol 29 (11) ◽  
pp. 2041015
Author(s):  
John L. Friedman ◽  
Nikolaos Stergioulas
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Maximum Mass ◽  
X Ray ◽  
Spectral Bands ◽  
Heaviest Elements ◽  
X Ray Binaries

The first inspiral of two neutron stars observed in gravitational waves was remarkably close, allowing the kind of simultaneous gravitational wave and electromagnetic observation that had not been expected for several years. Their merger, followed by a gamma-ray burst and a kilonova, was observed across the spectral bands of electromagnetic telescopes. These GW and electromagnetic observations have led to dramatic advances in understanding short gamma-ray bursts; determining the origin of the heaviest elements; and determining the maximum mass of neutron stars. From the imprint of tides on the gravitational waveforms and from observations of X-ray binaries, one can extract the radius and deformability of inspiraling neutron stars. Together, the radius, maximum mass, and causality constrain the neutron-star equation of state, and future constraints can come from observations of post-merger oscillations. We selectively review these results, filling in some of the physics with derivations and estimates.

The maximum mass of a neutron star

1977 ◽  
Vol 213 ◽  
pp. 234 ◽  
Author(s):  
P. Rastall
Keyword(s):  
Neutron Star ◽  
Maximum Mass

scholarly journals COMPUTATION OF NEUTRON STAR STRUCTURE USING MODERN EQUATION OF STATE

2006 ◽  
Vol 21 (07) ◽  
pp. 1555-1565 ◽  
Author(s):  
G. H. BORDBAR ◽  
M. HAYATI
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Equations Of State ◽  
Maximum Mass ◽  
Neutron Star Matter ◽  
Radio Pulsars ◽  
Good Consistency ◽  
The Given ◽  
Neutron Star Radius ◽  
Star Structure

Using the modern equations of state derived from microscopic calculations, we have calculated the neutron star structure. For the neutron star, we have obtained a minimum mass about 0.1 M⊙ which is nearly independent of the equation of state, and a maximum mass between 1.47 M⊙ and 1.98 M⊙ which is strongly dependent on the equation of state. It is shown that among the equations of state of neutron star matter which we have used, the stiffest one leads to higher maximum mass and radius and lower central density. It is seen that the given maximum mass for the Reid-93 equation of state shows a good consistency with the accurate observations of radio pulsars. We have indicated that the thickness of neutron star crust is very small compared to the predicted neutron star radius.

scholarly journals SU(2) Chiral Sigma Model Study of Phase Transition in Hybrid Stars

2003 ◽  
Vol 18 (30) ◽  
pp. 2135-2145 ◽  
Author(s):  
P. K. Jena ◽  
L. P. Singh
Keyword(s):  
Phase Transition ◽  
Neutron Star ◽  
Nuclear Matter ◽  
Quark Matter ◽  
Sigma Model ◽  
Maximum Mass ◽  
Model Study ◽  
Stable Solutions ◽  
Hybrid Stars ◽  
Matter Component

We use a modified SU(2) chiral sigma model to study nuclear matter component and simple bag model for quark matter constituting a neutron star. We also study the phase transition of nuclear matter to quark matter with the mixed phase characterized by two conserved charges in the interior of highly dense neutron stars. Stable solutions of Tolman–Oppenheimer–Volkoff equations representing hybrid stars are obtained with a maximum mass of 1.67M⊙ and radius around 8.9 km.

scholarly journals A cold neutron star in the transient low-mass X-ray binary HETE J1900.1–2455 after 10 yr of active accretion

2016 ◽  
Vol 465 (1) ◽  
pp. L10-L14 ◽  
Author(s):  
N. Degenaar ◽  
L.S. Ootes ◽  
M.T. Reynolds ◽  
R. Wijnands ◽  
D. Page
Keyword(s):  
Neutron Star ◽  
Cold Neutron ◽  
X Ray ◽  
Low Mass

scholarly journals Bayesian analysis of multimessenger M-R data with interpolated hybrid EoS

2021 ◽  
Vol 57 (11) ◽  
Author(s):  
A. Ayriyan ◽  
D. Blaschke ◽  
A. G. Grunfeld ◽  
D. Alvarez-Castillo ◽  
H. Grigorian ◽  
...  
Keyword(s):  
Neutron Star ◽  
Bayesian Analysis ◽  
Quark Matter ◽  
Equations Of State ◽  
Maximum Mass ◽  
Chemical Potentials ◽  
Parabolic Interpolation ◽  
Njl Model ◽  
Actual Outcome ◽  
Large Maximum

AbstractWe introduce a family of equations of state (EoS) for hybrid neutron star (NS) matter that is obtained by a two-zone parabolic interpolation between a soft hadronic EoS at low densities and a set of stiff quark matter EoS at high densities within a finite region of chemical potentials $$\mu _H< \mu < \mu _Q$$ μ H < μ < μ Q . Fixing the hadronic EoS as the APR one and choosing the color-superconducting, nonlocal NJL model with two free parameters for the quark phase, we perform Bayesian analyses with this two-parameter family of hybrid EoS. Using three different sets of observational constraints that include the mass of PSR J0740+6620, the tidal deformability for GW170817, and the mass-radius relation for PSR J0030+0451 from NICER as obligatory (set 1), while set 2 uses the possible upper limit on the maximum mass from GW170817 as an additional constraint and set 3 instead of the possibility that the lighter object in the asymmetric binary merger GW190814 is a neutron star. We confirm that in any case, the quark matter phase has to be color superconducting with the dimensionless diquark coupling approximately fulfilling the Fierz relation $$\eta _D=0.75$$ η D = 0.75 and the most probable solutions exhibiting a proportionality between $$\eta _D$$ η D and $$\eta _V$$ η V , the coupling of the repulsive vector interaction that is required for a sufficiently large maximum mass. We used the Bayesian analysis to investigate with the method of fictitious measurements the consequences of anticipating different radii for the massive $$2~M_\odot $$ 2 M ⊙ PSR J0740+6220 for the most likely equation of state. With the actual outcome of the NICER radius measurement on PSR J0740+6220 we could conclude that for the most likely hybrid star EoS would not support a maximum mass as large as $$2.5~M_\odot $$ 2.5 M ⊙ so that the event GW190814 was a binary black hole merger.

scholarly journals What Constraints on the Neutron Star Maximum Mass Can One Pose from GW170817 Observations?

2020 ◽  
Vol 893 (2) ◽  
pp. 146 ◽  
Author(s):  
Shunke Ai ◽  
He Gao ◽  
Bing Zhang
Keyword(s):  
Neutron Star ◽  
Maximum Mass
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