Gravitational-Wave Constraints on the Neutron-Star-Matter Equation of State

Annala, Eemeli; Gorda, Tyler; Kurkela, Aleksi; Vuorinen, Aleksi

doi:10.1103/physrevlett.120.172703

Cited by 942 publications

(1,044 citation statements)

References 69 publications

(124 reference statements)

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“…Different a and b values are found for different relativistic and nonrelativistic models, as one can verify for instance in Refs. [9,23,24]. Such a relation has also been derived in Ref.…”

Section: Still Regarding the Values Shown Insupporting

confidence: 57%

GW170817 constraints analyzed with Gogny forces and momentum-dependent interactions

et al. 2020

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A set of equations of state obtained from finite-range Gogny forces and momentum-dependent interactions is used to investigate the recent observation of gravitational waves from the binary neutron star merger GW170817 event. For this set of interactions, we have calculated the neutron star tidal deformabilities (related to the second Love number), the mass-radius diagram, and the moment of inertia (I). The I-Love relation has been verified. We also have found strong correlations among the tidal deformability of the canonical neutron star, its radius, and the derivatives of the nuclear symmetry energy at the saturation density. Most of the obtained results are located within the constraints of the tidal deformabilities extracted from the GW170817 detection.

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“…Different a and b values are found for different relativistic and nonrelativistic models, as one can verify for instance in Refs. [9,23,24]. Such a relation has also been derived in Ref.…”

Section: Still Regarding the Values Shown Insupporting

confidence: 57%

GW170817 constraints analyzed with Gogny forces and momentum-dependent interactions

et al. 2020

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“…model alone indicates that SGR J1745-2900 has as the most likely mass the canonical NS mass M = 1.4 M , and it should have a corresponding radius R 1.4 ≈ 9.4-12.3 km. This result obtained from electromagnetic data agrees with recent constraints obtained from gravitational wave observations that lead to R 1.4 13.5 km for hadronic stars (Annala et al 2018;De et al 2018;Abbott et al 2018;Most et al 2018). The above values would disfavour relativistic mean-field theory models, which usually lead to R 1.4 larger than 13.5 km (Fortin et al 2016).…”

Section: Discussionsupporting

confidence: 92%

Evidence for a Multipolar Magnetic Field in SGR J1745-2900 from X-Ray Light-curve Analysis

Lima

Coelho

Pereira

et al. 2020

ApJ

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SGR J1745-2900 was detected from its outburst activity in April 2013 and it was the first soft gamma repeater (SGR) detected near the center of the Galaxy (Sagittarius A * ). We use 3.5-year Chandra X-ray light-curve data to constrain some neutron star (NS) geometric parameters. We assume that the flux modulation comes from hot spots on the stellar surface. Our model includes the NS mass, radius, a maximum of three spots of any size, temperature and positions, and general relativistic effects. We find that the light-curve of SGR J1745-2900 could be described by either two or three hot spots. The ambiguity is due to the small amount of data, but our analysis suggests that one should not disregard the possibility of multi-spots (due to a multipolar magnetic field) in highly magnetized stars. For the case of three hot spots, we find that they should be large and have angular semi-apertures ranging from 16-67 degrees. The large size found for the spots points to a magnetic field with a nontrivial poloidal and toroidal structure (in accordance with magnetohydrodynamics investigations and NICER's recent findings for PSR J0030+0451) and is consistent with the small characteristic age of the star. Finally, we also discuss possible constraints on the mass and radius of SGR J1745-2900 and briefly envisage possible scenarios accounting for the 3.5-year evolution of SGR J1745-290 hot spots.

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“…That is, once two angles Θ and i and the opening angle ∆ψ are selected for the neutron star with M and R, one can calculate the time variation of the bolometric flux with ψ * (t) determined from Eq. (8), which corresponds to the light curve. As in Ref.…”

Section: Light Curves From Slowly Rotating Neutron Starsmentioning

confidence: 99%

Light curves from highly compact neutron stars with spot size effect

Sotani

2020

Phys. Rev. D

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We systematically examine light curves from a single hot spot on a slowly rotating neutron star with very high compactness, where the so-called invisible zone does not exist. In particular, we adopt three different shapes of hot spot and take into account the finite size effect of hot spot on the light curves. Then, we find that the brightening of flux occurs when the hot spot with small area crosses the opposite side to the observer, where the brightening becomes stronger as the area of hot spot decreases. Since this brightening happens only when a part of hot spot crosses the opposite side to the observer, one may constrain the neutron star geometry, i.e., the combination of an inclination angle, angle between the rotational axis and normal vector at the center of hot spot, and the opening angle of hot spot, if the brightening would be observed. In addition, by counting such a brightening in the light curves, one may know how many narrow bands of hot spot and/or spots with small area cross the opposite side to the observer.

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Gravitational-Wave Constraints on the Neutron-Star-Matter Equation of State

Cited by 942 publications

References 69 publications

GW170817 constraints analyzed with Gogny forces and momentum-dependent interactions

GW170817 constraints analyzed with Gogny forces and momentum-dependent interactions

Evidence for a Multipolar Magnetic Field in SGR J1745-2900 from X-Ray Light-curve Analysis

Light curves from highly compact neutron stars with spot size effect

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