scholarly journals Equation of state of dense matter and maximum mass of neutron stars

2003 ◽  
Vol 7 ◽  
pp. 249-249 ◽  
Author(s):  
P. Haensel
Keyword(s):  
Equation Of State ◽  
Neutron Stars ◽  
Dense Matter ◽  
Maximum Mass

scholarly journals Protoneutron stars and neutron stars

2000 ◽  
Vol 177 ◽  
pp. 663-664
Author(s):  
D. Gondek-Rosińska ◽  
P. Haensel ◽  
J. L. Zdunik
Keyword(s):  
Equation Of State ◽  
Neutron Stars ◽  
Dense Matter ◽  
Early Evolution ◽  
Maximum Mass ◽  
Standard Equation ◽  
Nuclear Incompressibility ◽  
Protoneutron Stars ◽  
Protoneutron Star

AbstractWe find constraints on minimum and maximum mass of ordinary neutron stars imposed by their early evolution (protoneutron star stage). We calculate models of protoneutron stars using a realistic standard equation of state of hot, dense matter valid for both supranuclear and subnuclear densities. Results for different values of the nuclear incompressibility are presented.

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.

scholarly journals Equation of state constraints for the cold dense matter inside neutron stars using the cooling tail method

2016 ◽  
Vol 591 ◽  
pp. A25 ◽  
Author(s):  
J. Nättilä ◽  
A. W. Steiner ◽  
J. J. E. Kajava ◽  
V. F. Suleimanov ◽  
J. Poutanen
Keyword(s):  
Equation Of State ◽  
Neutron Stars ◽  
State Constraints ◽  
Dense Matter ◽  
Cold Dense Matter

scholarly journals Equation of state of dense matter and the minimum mass of cold neutron stars

2002 ◽  
Vol 385 (1) ◽  
pp. 301-307 ◽  
Author(s):  
P. Haensel ◽  
J. L. Zdunik ◽  
F. Douchin
Keyword(s):  
Equation Of State ◽  
Neutron Stars ◽  
Cold Neutron ◽  
Dense Matter ◽  
Minimum Mass

scholarly journals The Effects of Nuclear Forces on the Maximum Mass Limit of Neutron Stars

1971 ◽  
Vol 46 ◽  
pp. 352-355
Author(s):  
Sachiko Tsuruta
Keyword(s):  
Equation Of State ◽  
Neutron Stars ◽  
Nuclear Interaction ◽  
Maximum Mass ◽  
Nuclear Forces ◽  
Mass Limit ◽  
Improved Model

The original models of neutron stars must be improved by including effects of nuclear interaction. This paper compares the models reached by various groups, and presents an improved model by the Kyoto group. The maximum mass varies between 0.2 M⊙ and 3 M⊙ in the various models. The Vγ model is recommended for use in the absence of further information on the equation of state at high densities.

Effect of the equation of state on the maximum mass of differentially rotating neutron stars

2016 ◽  
Vol 463 (3) ◽  
pp. 2667-2679 ◽  
Author(s):  
A. M. Studzińska ◽  
M. Kucaba ◽  
D. Gondek-Rosińska ◽  
L. Villain ◽  
M. Ansorg
Keyword(s):  
Equation Of State ◽  
Neutron Stars ◽  
Maximum Mass

scholarly journals Thermal properties of hot and dense matter: Influence of rapid rotation on protoneutron stars, hot neutron stars, and neutron star merger remnants

2021 ◽  
Vol 252 ◽  
pp. 05004
Author(s):  
Polychronis Koliogiannis ◽  
Charalampos Moustakidis
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Equations Of State ◽  
Interaction Model ◽  
Dense Matter ◽  
Baryon Density ◽  
Dense Nuclear Matter ◽  
Protoneutron Stars

The knowledge of the equation of state is a key ingredient for many dynamical phenomena that depend sensitively on the hot and dense nuclear matter, such as the formation of protoneutron stars and hot neutron stars. In order to accurately describe them, we construct equations of state at FInite temperature and entropy per baryon for matter with varying proton fractions. This procedure is based on the momentum dependent interaction model and state-of-the-art microscopic data. In addition, we investigate the role of thermal and rotation effects on microscopic and macroscopic properties of neutron stars, including the mass and radius, the frequency, the Kerr parameter, the central baryon density, etc. The latter is also connected to the hot and rapidly rotating remnant after neutron star merger. The interplay between these quantities and data from late observations of neutron stars, both isolated and in matter of merging, could provide useful insight and robust constraints on the equation of state of nuclear matter.

EQUATION OF STATE OF DENSE MATTER IN NEUTRON STARS

2008 ◽  
Author(s):  
SLAVOMÍR ČERNÝ ◽  
JIŘINA ŘÍKOVSKÁ STONE ◽  
ZDENĚK STUCHLÍK ◽  
STANISLAV HLEDÍK
Keyword(s):  
Equation Of State ◽  
Neutron Stars ◽  
Dense Matter
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