scholarly journals Neutron star-black hole mergers with a nuclear equation of state and neutrino cooling: Dependence in the binary parameters

2014 ◽  
Vol 90 (2) ◽  
Author(s):  
Francois Foucart ◽  
M. Brett Deaton ◽  
Matthew D. Duez ◽  
Evan O’Connor ◽  
Christian D. Ott ◽  
...  
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Equation Of State ◽  
Nuclear Equation Of State

scholarly journals Probing the Nuclear Equation of State from the Existence of a ∼2.6 M⊙ Neutron Star: The GW190814 Puzzle

Symmetry ◽  
2021 ◽  
Vol 13 (2) ◽  
pp. 183
Author(s):  
Alkiviadis Kanakis-Pegios ◽  
Polychronis S. Koliogiannis ◽  
Charalampos C. Moustakidis
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Equation Of State ◽  
Speed Of Sound ◽  
Compact Object ◽  
Dense Matter ◽  
High Mass ◽  
Nuclear Equation Of State ◽  
Dense Nuclear Matter ◽  
Low Mass

On 14 August 2019, the LIGO/Virgo collaboration observed a compact object with mass ∼2.59−0.09+0.08M⊙, as a component of a system where the main companion was a black hole with mass ∼23M⊙. A scientific debate initiated concerning the identification of the low mass component, as it falls into the neutron star–black hole mass gap. The understanding of the nature of GW190814 event will offer rich information concerning open issues, the speed of sound and the possible phase transition into other degrees of freedom. In the present work, we made an effort to probe the nuclear equation of state along with the GW190814 event. Firstly, we examine possible constraints on the nuclear equation of state inferred from the consideration that the low mass companion is a slow or rapidly rotating neutron star. In this case, the role of the upper bounds on the speed of sound is revealed, in connection with the dense nuclear matter properties. Secondly, we systematically study the tidal deformability of a possible high mass candidate existing as an individual star or as a component one in a binary neutron star system. As the tidal deformability and radius are quantities very sensitive on the neutron star equation of state, they are excellent counters on dense matter properties. We conjecture that similar isolated neutron stars or systems may exist in the universe and their possible future observation will shed light on the maximum neutron star mass problem.

scholarly journals BLACK HOLE-NEUTRON STAR MERGERS WITH A HOT NUCLEAR EQUATION OF STATE: OUTFLOW AND NEUTRINO-COOLED DISK FOR A LOW-MASS, HIGH-SPIN CASE

2013 ◽  
Vol 776 (1) ◽  
pp. 47 ◽  
Author(s):  
M. Brett Deaton ◽  
Matthew D. Duez ◽  
Francois Foucart ◽  
Evan O'Connor ◽  
Christian D. Ott ◽  
...  
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Equation Of State ◽  
High Spin ◽  
Nuclear Equation Of State ◽  
Low Mass

ERRATUM: “BLACK HOLE–NEUTRON STAR MERGERS WITH A HOT NUCLEAR EQUATION OF STATE: OUTFLOW AND NEUTRINO-COOLED DISK FOR A LOW-MASS, HIGH-SPIN CASE” (2013, ApJ, 776, 47)

2016 ◽  
Vol 824 (1) ◽  
pp. 62
Author(s):  
M. Brett Deaton ◽  
Matthew D. Duez ◽  
Francois Foucart ◽  
Evan O’Connor ◽  
Christian D. Ott ◽  
...  
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Equation Of State ◽  
High Spin ◽  
Nuclear Equation Of State ◽  
Low Mass

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 Extracting equation of state parameters from black hole-neutron star mergers: Aligned-spin black holes and a preliminary waveform model

2014 ◽  
Vol 89 (4) ◽  
Author(s):  
Benjamin D. Lackey ◽  
Koutarou Kyutoku ◽  
Masaru Shibata ◽  
Patrick R. Brady ◽  
John L. Friedman
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Neutron Star ◽  
Equation Of State

scholarly journals NEUTRON STAR VERSUS HEAVY-ION DATA: IS THE NUCLEAR EQUATION OF STATE HARD OR SOFT?

2008 ◽  
Author(s):  
JÜRGEN SCHAFFNER-BIELICH ◽  
IRINA SAGERT ◽  
MIRJAM WIETOSKA ◽  
CHRISTIAN STURM
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Heavy Ion ◽  
Nuclear Equation Of State ◽  
Star Versus
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