Saturation properties of hot asymmetric nuclear matter using M3Y effective nucleon-nucleon interaction

Seif, W. M.; Hashem, A. S.; Hassanien, R.N.

doi:10.1016/j.nuclphysa.2021.122142

Cited by 6 publications

(1 citation statement)

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“…These interactions are used frequently, with a high degree of confidence, to study nuclear structure [38,39], reactions [40][41][42][43][44], and decays [45][46][47]. Soft and stiff EOSs based on the two considered interactions, with incompressibility coefficient values ranging between 150 and 300 MeV, have been used in non-relativistic Hartree-Fock framework to investigate the symmetry [48,49] and saturation [50] properties of cold [32,51] and hot [28,52] NM, as well as β-stable neutron star matter [22,30,53] investigations. The mass-radius relation of neutron stars and massive pulsars and the different particle contributions to their core matter will be investigated in terms of the considered EOSs based on the realistic Michigan-three-Yukawa (M3Y)-Reid and M3Y-Paris NN interactions.…”

Section: Introductionmentioning

confidence: 99%

Mass–radius relation of neutron stars and massive pulsars with realistic equation of state

Seif,

Hashem,

Abualhamd

2024

J. Phys. G: Nucl. Part. Phys.

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We use up-to-date constraints on the mass and radius of 15 neutron star objects and pulsars, from electromagnetic and gravitational wave observables and different theoretical schemes, to extend the nuclear equation of state (EOS) based on realistic M3Y nucleon-nucleon interaction, which truly accounts for the low-density EOS of nuclear matter, to describe dense nuclear matter. The considered EOSs are employed to map the mass-radius profiles using the Tolman-Oppenheimer-Volkoff equations of hydrostatic equilibrium. We found that the EOSs from CDM3Y-230 to CDM3Y-270, with saturation incompressibility K0=230-270 MeV, successfully reproduce most of the recent constraints on the NS masses and radii. Based on both M3Y-Paris and M3Y-Reid NN interactions, these EOSs indicate radius of 11.67±0.34 km for the NS of 1.4Mʘmass, and the expected maximum NS mass (Mmax) to be 1.93±0.21 Mʘ. The upper limits of constraints indicated stiffer EOSs of K0=300 – 330 MeV, which have estimated 1arger radii of 12.29±0.14 km for NS (1.4Mʘ) and heavier Mmaxof 2.31±0.14 Mʘ. Increasing the stiffness of the employed EOS is found to increase the indicated maximum mass of NS, its radius and maximum compactness, the corecrust transition density, the speed of sound in its interior, and slightly the transition proton-fraction, but to decrease the abundance of the proton, muon, and electron over npeμ core matter of NS, as well as the estimated central density.

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