Asymmetric nuclear matter equation of state

Bombaci, Ignazio; Lombardo, U.

doi:10.1103/physrevc.44.1892

Cited by 402 publications

(423 citation statements)

References 36 publications

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“…It has been numerically demonstrated, by various microscopic calculations [58][59][60][61][62][63][64][65][66] adopting different realistic NN interactions, that the energy per particle of asymmetric nuclear matter can be accurately reproduced by the following relation:…”

Section: Resultsmentioning

confidence: 99%

Comparative study of three-nucleon force models in nuclear matter

et al. 2015

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We calculate the energy per particle of symmetric nuclear matter and pure neutron matter using the microscopic many-body Brueckner-Hartree-Fock (BHF) approach and employing the Argonne V18 (AV18) nucleon-nucleon (NN) potential supplemented with two different three-nucleon force models recently constructed to reproduce the binding energy of 3 H, 3 He, and 4 He nuclei as well as the neutron-deuteron doublet scattering length. We find that none of these new three-nucleon force models is able to reproduce simultaneously the empirical saturation point of symmetric nuclear matter and the properties of three-and four-nucleon systems.

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Section: Resultsmentioning

confidence: 99%

Comparative study of three-nucleon force models in nuclear matter

et al. 2015

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“…Realistic parameter sets should have a U N below the KaoS constraint up to densities of n ∼ (2 − 3) n 0 . The TM1 [61] parametrization as well as the BruecknerHartree-Fock approximation (BHF) [62][63][64][65] fulfill this requirement. For a RMF model with n 0 = 0.17 fm −3 and K 0 = 220 MeV, we arrive at m * /m = (0.53 − 0.65) for n ∼ (2 − 3) n 0 while for K 0 = 250 MeV we obtain m * /m = (0.54 − 0.67) for the same density range.…”

Section: Maximum Neutron Star Massesmentioning

confidence: 99%

Soft nuclear equation-of-state from heavy-ion data and implications for compact stars

Sagert

Tolós

Chatterjee³

et al. 2012

Phys. Rev. C

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Measurements of kaon production at subthreshold energies in heavy-ion collisions point to a soft nuclear equation-of-state for densities up to 2-3 times nuclear matter saturation density. We apply these results to study the implications on compact star properties, especially in the context of the recent measurement of the two solar mass pulsar PSR J1614-2230. The implications are twofold: Firstly, the heavy-ion results constrain nuclear matter at densities relevant to light neutron stars. Hence, a radius measurement could provide information about the density dependence of the symmetry energy which is a crucial quantity in nuclear physics. Secondly, the information on the nucleon potential obtained from the analysis of the heavy-ion data can be combined with restrictions from causality on the nuclear equation-of-state. From this we can derive a limit for the highest allowed compact star mass of three solar masses.

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“…in a regime where the EoS is poorly constrained by nuclear data and experiments. The nuclear symmetry energy is thus one of the most relevant quantities to control the composition, and the pressure of β-stable nuclear matter [4,5], and therefore many NS attributes such as the radius, moment of inertia, and crustal properties [6].…”

Section: Introductionmentioning

confidence: 99%

The Hyperon Puzzle in Neutron Stars

Bombaci

2017

Proceedings of the 12th International Conference on Hypernuclear and Strange Particle Physics (HYP2015)

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The so called hyperon puzzle, i.e. the difficulty to reconcile the measured masses of neutron stars (NSs) with the presence of hyperons in their interiors, is one of the hot topics in astrophysics which is stimulating copious experimental and theoretical research in hypernuclear physics. After illustrating the origin of the hyperon puzzle, I discuss some of its possible solutions, and particularly those related to the role of hyperonic two-and three-body interactions on the equation of state of dense matter. Afterward, I discuss a possibility to circumvent the hyperon puzzle allowing for the presence of strangeness in NSs in the form of deconfined strange quark matter, and thus considering the so called quark stars, i.e. hybrid stars or strange stars. Finally I discuss the astrophysical consequences of the possible conversion process of an hadronic star to a quark star.

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Asymmetric nuclear matter equation of state

Cited by 402 publications

References 36 publications

Comparative study of three-nucleon force models in nuclear matter

Comparative study of three-nucleon force models in nuclear matter

Soft nuclear equation-of-state from heavy-ion data and implications for compact stars

The Hyperon Puzzle in Neutron Stars

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