Publisher's Note: Neutron star properties and the equation of state of neutron-rich matter [Phys. Rev. C 74, 025808 (2006)]

Krastev, Plamen G.; Sammarruca, Francesca

doi:10.1103/physrevc.74.039901

Cited by 51 publications

(87 citation statements)

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“…The value of r (= R), where the pressure vanishes defines the surface of the star. We solve the above equations to study the structural properties of a static neutron star using the EoS derived for the electrically charge neutral hyperonic dense matter [26,27].…”

Section: Stellar Equationsmentioning

confidence: 99%

Attributes of a rotating neutron star with a hyperon core

2008

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We study the effect of rotation on global properties of neutron star with a hyperon core in an effective chiral model with varying nucleon effective mass within a mean field approach. The resulting gross properties of the rotating compact star sequences are then compared and analyzed with other theoretical predictions and observations from neutron stars. The maximum mass of the compact star predicted by the model lies in the range (1.4 − 2.4) M⊙ at Kepler frequency ΩK , which is consistent with recent observation of high mass stars thereby reflecting the sensitivity of the underlying nucleon effective mass in the dense matter EoS. We also discuss the implications of the experimental constraints from the flow data from heavy-ion collisions on the global properties of the rotating neutron stars.

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Section: Stellar Equationsmentioning

confidence: 99%

Attributes of a rotating neutron star with a hyperon core

2008

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“…non-relativistic Brueckner (BHF) as well as for relativistic Brueckner (DBHF) calculations [12,38]. The BHF calculations differ essentially in the usage of different 3-body-forces (3-BFs).…”

Section: Pos(cpod07)060mentioning

confidence: 99%

The high density equation of state: constraints from accelerators

Fuchs¹

2008

Proceedings of Critical Point and Onset of Deconfinement - 4th International Workshop — PoS(CPOD07)

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The nuclear equation of state (EoS) at high densities and/or extreme isospin is one of the longstanding problems of nuclear physics. In the last years substantial progress has been made to constrain the EoS both, from the astrophysical side and from accelerator based experiments. Heavy ion experiments support a soft EoS at moderate densities while the possible existence of high mass neutron star observations favors a stiff EoS. Ab initio calculations for the nuclear manybody problem make predictions for the density and isospin dependence of the EoS far away from the saturation point. Both, the constraints from astrophysics and accelerator based experiments are shown to be in agreement with the predictions from many-body theory. Critical Point and Onset of Deconfinement 4th International Workshop

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“…For neutron rich matter, the tensor effect in realistic NN interaction is suppressed largely in the T = 1 isospin channel [27,[31][32][33]. Therefore, it is enough to explicitly consider only the short-range correlation in neutron rich matter.…”

Section: Introductionmentioning

confidence: 99%

“…Akmal et al used the hyper-netted chain-summation technique in the non-relativistic variational method [23] and the AV18 potential [24] to calculate the EOS of neutron rich matter [25] with a three-body force. Krastev and Sammarruca adopted the relativistic Brueckner-HartreeFock (RBHF) [26] theory to study the properties of neutron stars with Bonn potentials [27].…”

Section: Introductionmentioning

confidence: 99%

“…Furthermore, the calculation procedures of the ab initio aforementioned methods, when they were applied to neutron star matter in β equilibrium, are complicated, therefore, the equations of β equilibrium are usually solved with various approximations instead of selfconsistence treatments [25,27]. Hence, the intention of this work is to apply the RVC method to calculate the EOSs of neutron star matter in β equilibrium self-consistently and use these EOSs to study the properties of neutron stars with realistic NN interaction, Bonn potentials.…”

Section: Introductionmentioning

confidence: 99%

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Neutron stars within a relativistic central variational method

Shen

Toki

2017

Phys. Rev. C

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The properties of neutron stars are investigated within the relativistic central variational method by using a realistic nucleon-nucleon (N N ) interaction. The strong repulsion of realistic N N interactions at short distances is treated by a Jastrow central correlation function, whose form is completely determined through minimization of the total energy of the nuclear many-body system.The relativistic Hartree-Fock wave functions are chosen as the trial wave function. In this framework, the equation of state of the neutron star matter in β equilibrium is obtained self-consistently.We further determine the properties of neutron stars via the Tolman-Oppenheimer-Volkoff equation using Bonn A, B, and C potentials. The maximum masses of neutron stars with these realistic potentials are around 2.18M ⊙ and their corresponding radii are around 11 km. These results are in accordance with the calculations of the relativistic Brueckner-Hartree-Fock theory with the same potentials. Furthermore, we also find that the splitting of proton-neutron effective masses will be reversed at high density in the neutron star matter, which are caused by the contribution of short-range correlation on kinetic energy.

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Publisher's Note: Neutron star properties and the equation of state of neutron-rich matter [Phys. Rev. C 74, 025808 (2006)]

Cited by 51 publications

References 0 publications

Attributes of a rotating neutron star with a hyperon core

Attributes of a rotating neutron star with a hyperon core

The high density equation of state: constraints from accelerators

Neutron stars within a relativistic central variational method

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