Nucleon effective mass in symmetric nuclear matter from the extended Brueckner-Hartree-Fock approach

2012 ◽  
Vol 36 (6) ◽  
pp. 513-518 ◽  
Author(s):  
Sheng-Xin Gan ◽  
Wei Zuo ◽  
U. Lombardo
2018 ◽  
Vol 609 ◽  
pp. A128 ◽  
Author(s):  
Ignazio Bombaci ◽  
Domenico Logoteta

Aims. We report a new microscopic equation of state (EOS) of dense symmetric nuclear matter, pure neutron matter, and asymmetric and β-stable nuclear matter at zero temperature using recent realistic two-body and three-body nuclear interactions derived in the framework of chiral perturbation theory (ChPT) and including the Δ(1232) isobar intermediate state. This EOS is provided in tabular form and in parametrized form ready for use in numerical general relativity simulations of binary neutron star merging. Here we use our new EOS for β-stable nuclear matter to compute various structural properties of non-rotating neutron stars. Methods. The EOS is derived using the Brueckner–Bethe–Goldstone quantum many-body theory in the Brueckner–Hartree–Fock approximation. Neutron star properties are next computed solving numerically the Tolman–Oppenheimer–Volkov structure equations. Results. Our EOS models are able to reproduce the empirical saturation point of symmetric nuclear matter, the symmetry energy Esym, and its slope parameter L at the empirical saturation density n0. In addition, our EOS models are compatible with experimental data from collisions between heavy nuclei at energies ranging from a few tens of MeV up to several hundreds of MeV per nucleon. These experiments provide a selective test for constraining the nuclear EOS up to ~4n0. Our EOS models are consistent with present measured neutron star masses and particularly with the mass M = 2.01 ± 0.04 M⊙ of the neutron stars in PSR J0348+0432.


2009 ◽  
Vol 18 (05n06) ◽  
pp. 1191-1205
Author(s):  
A. B. SANTRA ◽  
U. LOMBARDO

We have calculated the saturation observables of symmetric nuclear matter and nuclear symmetry energy in the framework of Brueckner-Hartree-Fock (BHF) formalism with Bonn-B potential as two-body interaction, including modification of hadronic parameter inside nuclear medium. We have found that it is possible to understand all the saturation observables of symmetric nuclear matter by incorporating in-medium modification of the parameters of sigma meson alone. Linear density dependent reduction of σ-nucleon coupling constant by about 6.8% and density independent reduction σ-meson mass by about 3.5% is sufficient to understand nuclear matter saturation observables. We find with the calculated symmetry energy that neutron skin thickness of 208Pb is 0.20 fm and the radius of 1.4 solar mass neutron stars as 11.98 ± 0.75 km.


2015 ◽  
Vol 91 (2) ◽  
Author(s):  
Li Juan Jiang ◽  
Shen Yang ◽  
Jian Min Dong ◽  
Wen Hui Long

2019 ◽  
Vol 28 (05) ◽  
pp. 1950034
Author(s):  
Prafulla K. Panda ◽  
Constança Providência ◽  
Steven A. Moszkowski ◽  
Henrik Bohr ◽  
João da Providência

We generalize the Bogoliubov quark-meson coupling (QMC) model to also include hyperons. The hyperon-[Formula: see text]-meson couplings are fixed by the model and the hyperon-[Formula: see text]-meson couplings are fitted to the hyperon potentials in symmetric nuclear matter. The present model predicts neutron stars with masses above 2[Formula: see text] and the radius of a 1.4[Formula: see text] star [Formula: see text]14[Formula: see text]km. In the most massive stars, bags overlap at the core of the star, and this may be interpreted as a transition to deconfined quark matter.


2004 ◽  
Vol 604 (3-4) ◽  
pp. 170-174 ◽  
Author(s):  
Zhong-Yu Ma ◽  
Jian Rong ◽  
Bao-Qiu Chen ◽  
Zhi-Yuan Zhu ◽  
Hong-Qiu Song

1991 ◽  
Vol 17 (6) ◽  
pp. 887-900 ◽  
Author(s):  
T Shamsunnahar ◽  
S Saha ◽  
K Kabir ◽  
L M Nath

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