Systematic analysis of the impacts of symmetry energy parameters on neutron star properties

Patra, N. K.; Venneti, Anagh; Imam, S.; Mukherjee, Arunava; Agrawal, B. K.

doi:10.1103/physrevc.107.055804

Cited by 9 publications

(2 citation statements)

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“…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). If the observational bounds are credible, then stiffer EoS are needed to support the NS with a higher mass 2M e .…”

Section: Introductionmentioning

confidence: 67%

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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Section: Introductionmentioning

confidence: 67%

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

Nashed

2023

ApJ

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“…Pradhan et al (2022) reported how the effective nucleon mass (m å ) at saturation is correlated with the f-mode frequencies for a set of EOSs generated within the RMF formalism. A strong correlation of the stellar oscillation frequencies with symmetry energy parameters like J sym,0 , K sym,0 , L sym,0 , and so on would allow us to infer the composition of matter at very high densities in the NS interior (Patra et al 2023).…”

Section: Introductionmentioning

confidence: 99%

Analysis of Neutron Star f-mode Oscillations in General Relativity with Spectral Representation of Nuclear Equations of State

Guha Roy,

Malik,

Bhattacharya

et al. 2024

ApJ

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We study quasi-normal f-mode oscillations in neutron star (NS) interiors within a linearized general relativistic formalism. We utilize approximately 9000 nuclear equations of state (EOSs) using spectral representation techniques, incorporating constraints on nuclear saturation properties, chiral effective field theory for pure neutron matter, and perturbative quantum chromodynamics for densities pertinent to NS cores. The median values of the f-mode frequency, ν f (damping time, τ f ) for NSs with masses ranging from 1.4 to 2.0 M ⊙ lie between 1.80 and 2.20 kHz (0.13–0.22 s) for our entire EOS set. Our study reveals a weak correlation between f-mode frequencies and individual nuclear saturation properties, prompting the necessity for more intricate methodologies to unveil multiparameter relationships. We observe a robust linear relationship between the radii and f-mode frequencies for different NS masses. Leveraging this correlation alongside NICER observations of PSR J0740+6620 and PSR J0030+0451, we establish constraints that exhibit partial and minimal overlap for observational data from Riley et al. and Miller et al., respectively, with our nucleonic EOS data set. Moreover, NICER data align closely with the radius and frequency values for a few hadron–quark hybrid EOS models. This indicates the need to consider additional exotic particles such as deconfined quarks at suprasaturation densities. We conclude that future observations of the radius or f-mode frequency for more than one NS mass, particularly at the extremes of the viable NS mass scale, would either rule out nucleon-only EOSs or provide definitive evidence in its favor.

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