The Nuclear Matter Density Functional under the Nucleonic Hypothesis

Thi, Hoa Dinh; Mondal, C.; Gulminelli, F.

doi:10.3390/universe7100373

Cited by 30 publications

(5 citation statements)

References 71 publications

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“…These results imply that the neutron star matter EoS should not be too stiff at densities below twice the saturation density n 0 = 0.15 fm −3 (roughly corresponding to the central density of an NS with M = 1.4 M ), but has to be stiff enough at higher densities to allow for a maximum mass above 2.0 M . These new constraints on the NS mass-radius relation can be fulfilled within the purely nucleonic scenario for the NS interiors [3]. At the same time, approaches based on realistic nuclear interactions imply appearance of hyperons in the NS interiors, which softens EoS of nuclear matter and lowers the NS maximum mass M max .…”

Section: Introductionmentioning

confidence: 92%

Recovering the Conformal Limit of Color Superconducting Quark Matter within a Confining Density Functional Approach

Ivanytskyi

Blaschke

2022

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We generalize a recently proposed confining relativistic density-functional approach to the case of density-dependent vector and diquark couplings. The particular behavior of these couplings is motivated by the non-perturbative gluon exchange in dense quark matter and provides the conformal limit at asymptotically high densities. We demonstrate that this feature of the quark matter EoS is consistent with a significant stiffness in the density range typical for the interiors of neutron stars. In order to model these astrophysical objects, we construct a family of hybrid quark-hadron EoSs of cold stellar matter. We also confront our approach with the observational constraints on the mass–radius relation of neutron stars and their tidal deformabilities and argue in favor of a quark matter onset at masses below 1.0M⊙.

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Section: Introductionmentioning

confidence: 92%

Recovering the Conformal Limit of Color Superconducting Quark Matter within a Confining Density Functional Approach

Ivanytskyi

Blaschke

2022

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“…The BNS signals emitted by coalescing neutron stars are presumed to be observed more frequently in the upcoming LIGO-Virgo-KAGRA runs and prospective detectors, such as the Einstein Telescope (Punturo et al 2010) and Cosmic Explorer (Reitze et al 2019). The unexpected limitations on the EoS promised by gravitational wave astronomy, as revealed by a thorough analysis of gravitational wave parameter estimation, have prompted numerous theoretical investigations of neutron star characteristics (Abbott et al 2017(Abbott et al , 2020aMalik et al 2018;De et al 2018;Nashed & El Hanafy 2017;Liliani et al 2021;Forbes et al 2019;Landry & Essick 2019;Piekarewicz & Fattoyev 2019;Biswas et al 2021a;Dinh Thi et al 2021) (Riley et al 2021) were noted for the heavier pulsar PSR J0740 +6620. The lower bound on the maximum NS mass for the black-widow pulsar PSR J0952-0607 (Romani et al 2022) surpasses any prior measurements, including M max = M 2.35 0.17   for PSR J2215-5135 (Linares et al 2018;Patra et al 2023).…”

Section: Introductionmentioning

confidence: 99%

The Effect of f(R, T) Modified Gravity on the Mass and Radius of Pulsar HerX1

Nashed

2023

ApJ

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Millisecond pulsars are the perfect testable to examine potential matter-geometry coupling and its physical consequences in the context of the recent Neutron Star Interior Composition Explorer discoveries. We apply the field equations of modified gravity, f(R, T) = R + α T, to a spherically symmetric spacetime, where R is the Ricci scalar, α is a dimensional parameter, and T is the matter of the geometry. Five unknown functions are present in the output system of differential equations, which consists of three equations. To close the system, we make explicit assumptions about the anisotropy and the radial metric potential, g rr . We then solve the output differential equations and derive the explicit forms of the components of the energy-momentum tensor, i.e., density, radial, and tangential pressures. We look into the possibility that all of the physical parameters in the star can be reexpressed in terms of α and the compactness parameters, C = 2 GM Rc−2. We show that, for a given mass, the size permitted by Einstein’s general relativity is less due to the matter-geometry coupling in f(R, T). The validity of the hypothesis was validated by observations from an extra 21 pulsars. To achieve a surface density that is compatible with a neutron core at nuclear saturation density, the mass–radius curve enables masses up to 3.35M ⊙. We emphasize that although there is no assumption of an equation of state, the model fits well with a linear behavior. When comparing the surface densities of these 20 pulsars, we divided them into three groups. We show that these three groups are compatible with neutron cores.

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“…The BNS signals emitted from coalescing neutron stars are likely to be observed more frequently in the upcoming runs of LIGO-Virgo-KAGRA and the future detectors, e.g., Einstein Telescope [10] and Cosmic Explorer [11]. The unprecedented constraints on the EoS promised by gravitational wave astronomy through the detailed analysis of gravitational wave parameter estimation has triggered many theoretical investigations of the properties of neutron star [9,[12][13][14][15][16][17][18][19][20]. Recently, two different groups of Neutron star Interior Composition Explorer (NICER) X-ray telescopes provided neutron star's mass and radius simultaneously for PSR J0030+0451 with R = 13.02 +1.…”

Section: Introductionmentioning

confidence: 99%