scholarly journals Massive neutron star with strangeness in a relativistic mean-field model with a high-density cutoff

2018 ◽  
Vol 97 (1) ◽  
Author(s):  
Ying Zhang ◽  
Jinniu Hu ◽  
Peng Liu
Keyword(s):  
Neutron Star ◽  
Field Model ◽  
Mean Field ◽  
High Density ◽  
Mean Field Model ◽  
Relativistic Mean Field ◽  
Massive Neutron Star

IMPACTS OF PARAMETERS ADJUSTMENT OF RELATIVISTIC MEAN FIELD MODEL ON NEUTRON STAR PROPERTIES

2011 ◽  
Vol 20 (05) ◽  
pp. 1271-1285 ◽  
Author(s):  
KASMUDIN ◽  
A. SULAKSONO
Keyword(s):  
Neutron Star ◽  
Reasonable Agreement ◽  
Field Model ◽  
Mean Field ◽  
Effective Field ◽  
Radiation Measurement ◽  
Mean Field Model ◽  
Relativistic Mean Field ◽  
The Moment ◽  
Rmf Model

Analysis of the parameters adjustment effects in isovector as well as in isoscalar sectors of effective field based relativistic mean field (E-RMF) model in the symmetric nuclear matter and neutron-rich matter properties has been performed. The impacts of the adjustment on slowly rotating neutron star are systematically investigated. It is found that the mass–radius relation obtained from adjusted parameter set G2** is compatible not only with neutron stars masses from 4U 0614+09 and 4U 1636-536, but also with the ones from thermal radiation measurement in RX J1856 and with the radius range of canonical neutron star of X7 in 47 Tuc, respectively. It is also found that the moment inertia of PSR J073-3039A and the strain amplitude of gravitational wave at the Earth's vicinity of PSR J0437-4715 as predicted by the E-RMF parameter sets used are in reasonable agreement with the extracted constraints of these observations from isospin diffusion data.

scholarly journals Neutron star matter equation of state including d*-hexaquark degrees of freedom

2020 ◽  
Vol 638 ◽  
pp. A40
Author(s):  
A. Mantziris ◽  
A. Pastore ◽  
I. Vidaña ◽  
D. P. Watts ◽  
M. Bashkanov ◽  
...  
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Degrees Of Freedom ◽  
Field Model ◽  
Mean Field ◽  
The Other ◽  
Neutron Star Matter ◽  
Mean Field Model ◽  
Relativistic Mean Field ◽  
Walecka Model

We present the extension of a previous study where, assuming a simple free bosonic gas supplemented with a relativistic mean-field model to describe the pure nucleonic part of the equation of state, we studied the consequences that the first non-trivial hexaquark d*(2380) could have on the properties of neutron stars. Compared to that exploratory work, we employ a standard non-linear Walecka model including additional terms that describe the interaction of the d*(2380) di-baryon with the other particles of the system through the exchange of σ- and ω-meson fields. Our results show that the presence of the d*(2380) leads to maximum masses compatible with recent observations of ∼2 M⊙ millisecond pulsars if the interaction of the d*(2380) is slightly repulsive or the d*(2380) does not interact at all. An attractive interaction makes the equation of state too soft to be able to support a 2 M⊙ neutron star whereas an extremely repulsive one induces the collapse of the neutron star into a black hole as soon as the d*(2380) appears.

EVOLUTION OF SHELL STRUCTURE IN NUCLEI

2011 ◽  
Vol 20 (08) ◽  
pp. 1663-1675 ◽  
Author(s):  
A. BHAGWAT ◽  
Y. K. GAMBHIR
Keyword(s):  
Shell Structure ◽  
Crucial Role ◽  
Field Model ◽  
Mean Field ◽  
Mass Region ◽  
The Other ◽  
Mean Field Model ◽  
Relativistic Mean Field ◽  
Shell Closures ◽  
Low Mass

Systematic investigations of the pairing and two-neutron separation energies which play a crucial role in the evolution of shell structure in nuclei, are carried out within the framework of relativistic mean-field model. The shell closures are found to be robust, as expected, up to the lead region. New shell closures appear in low mass region. In the superheavy region, on the other hand, it is found that the shell closures are not as robust, and they depend on the particular combinations of neutron and proton numbers. Effect of deformation on the shell structure is found to be marginal.

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