scholarly journals Reconstruction of the neutron star equation of state from w -quasinormal modes spectra with a piecewise polytropic meshing and refinement method

2019 ◽  
Vol 99 (10) ◽  
Author(s):  
Juan Mena-Fernández ◽  
Luis Manuel González-Romero
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Quasinormal Modes ◽  
Refinement Method

scholarly journals Waveform systematics in the gravitational-wave inference of tidal parameters and equation of state from binary neutron-star signals

2021 ◽  
Vol 103 (12) ◽  
Author(s):  
Rossella Gamba ◽  
Matteo Breschi ◽  
Sebastiano Bernuzzi ◽  
Michalis Agathos ◽  
Alessandro Nagar
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Gravitational Wave ◽  
Binary Neutron Star

scholarly journals Neutron Star Equation of State in Light of GW190814

2020 ◽  
Vol 125 (26) ◽  
Author(s):  
Hung Tan ◽  
Jacquelyn Noronha-Hostler ◽  
Nico Yunes
Keyword(s):  
Neutron Star ◽  
Equation Of State

Ferromagnetism in neutron matter and its implication for the neutron star equation of state

2011 ◽  
Author(s):  
J. P. W. Diener ◽  
F. G. Scholtz ◽  
Ersin Göğüş ◽  
Ünal Ertan ◽  
Tomaso Belloni
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Matter

scholarly journals Neutron star properties and the equation of state for the core

2017 ◽  
Vol 599 ◽  
pp. A119 ◽  
Author(s):  
J. L. Zdunik ◽  
M. Fortin ◽  
P. Haensel
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
The Core

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 Neutron star masses

2012 ◽  
Vol 8 (S291) ◽  
pp. 146-146
Author(s):  
David Nice
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Nuclear Matter ◽  
Observational Data ◽  
Mass Distribution ◽  
Binary Star ◽  
Star Mass ◽  
Star Evolution ◽  
Neutron Star Mass ◽  
Present Understanding

AbstractNeutron star masses can be inferred from observations of binary pulsar systems, particularly by the measurement of relativistic phenomena within these orbits. The observed distribution of masses can be used to infer or constrain the equation of state for nuclear matter and to study astrophysical processes such as supernovae and binary star evolution. In this talk, I will review our present understanding of the neutron star mass distribution with an emphasis on the observational data.

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