Complexity and boost symmetry

Zhao, Ying

doi:10.1103/physrevd.98.086011

Cited by 43 publications

(53 citation statements)

References 27 publications

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“…Different groups have already exploited the knowledge of tidal deformability in GW170817 to estimate radii of merger components. An analytical approach was prescribed to estimate the radius of a 1.4 M ⊙ neutron star relating the value of tidal deformability obtained from GW17017 (Zhao & Lattimer 2018). We extend this prescription to estimate the radius of a neutron star in the mass range 1.1M ⊙ M 1.6M ⊙ .…”

Section: Resultsmentioning

confidence: 99%

“…The Neutron Star Composition Explorer (NICER) mission in the space station is devoted to the estimation of neutron star radius observing x-rays from rotation powered pulsars. However, the extracted value of effective tidal deformability 70 ≤ Λ ≤ 720 from GW170817 provides important information about radii of neutron stars involved in the binary neutron star merger event GW170817 (Abbott et al 2018;Most et al 2018;Fattoyev et al 2018;Raithel et al 2018;De et al 2018;Zhao & Lattimer 2018) for tidal deformability strongly correlates with radius of a neutron star. All those calculations indicate that the radii of 1.4 M ⊙ neutron stars could be 9 ≤ R/km ≤ 14.…”

Section: Introductionmentioning

confidence: 99%

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Properties of Binary Components and Remnant in GW170817 Using Equations of State in Finite Temperature Field Theory Models

Soma

Bandyopadhyay

2020

ApJ

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We investigate gross properties of merger components and remnant in GW170817 using equations of state (EoSs) within the finite temperature field theoretical models. We also adopt finite temperature equations of state in the density dependent hadron field theory such as DD2 EoS and Banik, Hempel and Bandyopadhyay (BHB) EoS involving Λ hyperons interacting via Φ meson popularly known as BHBΛφ EoS. Properties of merger components are studied using zero temperature EoSs. Particularly we investigate tidal deformabilities and radii of merger components in light of GW170817. An analytical expression relating the radius of merger components and the combined tidal deformability is obtained for binary neutron star masses in the range 1.1M ⊙ M 1.6M ⊙ . The upper bound on the tidal deformability gives the upper bound on the radius of merger components 13 km. Next the role of finite temperature on the merger remnant is explored. In this case, we investigate the gravitational and baryon mass, radius, Kepler frequency and moment of inertia of the rigidly rotating remnant for different EoSs at fixed entropy per baryon. The remnant radius is enlarged due to thermal effects compared with the zero temperature case. Consequently it is found that the Kepler frequency is much lower at higher entropy per baryon than that of the case at zero temperature.

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Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Properties of Binary Components and Remnant in GW170817 Using Equations of State in Finite Temperature Field Theory Models

Soma

Bandyopadhyay

2020

ApJ

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“…In addition, the relationship R 1.4 = (13.4 ± 0.1)(Λ/800) 1/6 was suggested in ref. [317]. However, a linear relationship between R 1.4 and Λ 1.4 appears when the parameters of E sym (ρ) are restricted to their current uncertainty ranges in ref.…”

Section: Gw170817 Implications On the Radii Of Neutron Starsmentioning

confidence: 99%

Towards understanding astrophysical effects of nuclear symmetry energy

et al. 2019

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Determining the Equation of State (EOS) of dense neutron-rich nuclear matter is a shared goal of both nuclear physics and astrophysics. Except possible phase transitions, the density dependence of nuclear symmetry Esym(ρ) is the most uncertain part of the EOS of neutron-rich nucleonic matter especially at supra-saturation densities. Much progresses have been made in recent years in predicting the symmetry energy and understanding why it is still very uncertain using various microscopic nuclear many-body theories and phenomenological models. Simultaneously, significant progresses have also been made in probing the symmetry energy in both terrestrial nuclear laboratories and astrophysical observatories. In light of the GW170817 event as well as ongoing or planned nuclear experiments and astrophysical observations probing the EOS of dense neutron-rich matter, we review recent progresses and identify new challenges to the best knowledge we have on several selected topics critical for understanding astrophysical effects of the nuclear symmetry energy.PACS. 2 6.60.Kp Contents B.A Li, P.G. Krastev, D.H. Wen and N.B. Zhang: Astrophysical Effects of Nuclear Symmetry Energy 5.2.2 Predicted correlation strength between the radii of neutron stars and the symmetry energy from low to high densities 32 5.2.3 Predicted effects of the symmetry energy on the tidal deformability of neutron stars 33 5.3 Post-GW170817 analyses of tidal deformability and radii of neutron stars as well as constraints on the nuclear EOS and symmetry energy . . . 34 5.3.

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“…To explore consequences of the many predictions of these models at supra-nuclear densities, piecewise polytropic EoSs that are causal have also been extensively used to map out the range of pressure vs density relations (EoSs) that are consistent with neutron star phenomenology [35][36][37][38]. The viability of these EoSs at supra-nuclear densities necessarily depends on the growing neutron star data to be detailed below.…”

Section: Introductionmentioning

confidence: 99%

Treating quarks within neutron stars

et al. 2019

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Neutron star interiors provide the opportunity to probe properties of cold dense matter in the QCD phase diagram. Utilizing models of dense matter in accord with nuclear systematics at nuclear densities, we investigate the compatibility of deconfined quark cores with current observational constraints on the maximum mass and tidal deformability of neutron stars. We explore various methods of implementing the hadron-to-quark phase transition, specifically, first-order transitions with sharp (Maxwell construction) and soft (Gibbs construction) interfaces, and smooth crossover transitions. We find that within the models we apply, hadronic matter has to be stiff for a first-order phase transition and soft for a crossover transition. In both scenarios and for the equations of state we employed, quarks appear at the center of pre-merger neutron stars in the mass range ≈ 1.0 − 1.6 M , with a squared speed of sound c 2 QM 0.4 characteristic of strong repulsive interactions required to support the recently discovered neutron star masses ≥ 2 M . We also identify equations of state and phase transition scenarios that are consistent with the bounds placed on tidal deformations of neutron stars in the recent binary merger event GW170817. We emphasize that distinguishing hybrid stars with quark cores from normal hadronic stars is very difficult from the knowledge of masses and radii alone, unless drastic sharp transitions induce distinctive disconnected hybrid branches in the mass-radius relation.

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Complexity and boost symmetry

Cited by 43 publications

References 27 publications

Properties of Binary Components and Remnant in GW170817 Using Equations of State in Finite Temperature Field Theory Models

Properties of Binary Components and Remnant in GW170817 Using Equations of State in Finite Temperature Field Theory Models

Towards understanding astrophysical effects of nuclear symmetry energy

Treating quarks within neutron stars

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