Structural evolution and shape transition in even-even Hf-isotopes within the relativistic mean-field approach

2022 ◽  
pp. 122380
Monalisa Das ◽  
N. Biswal ◽  
R.N. Panda ◽  
M. Bhuyan
2008 ◽  
Vol 17 (09) ◽  
pp. 1765-1773 ◽  

The microscopic properties and superfluidity of the inner crust in neutron stars are investigated in the framework of the relativistic mean field(RMF) model and BCS theory. The Wigner-Seitz(W-S) cell of inner crust is composed of neutron-rich nuclei immersed in a sea of dilute, homogeneous neutron gas. The pairing properties of nucleons in the W-S cells are treated in BCS theory with Gogny interaction. In this work, we emphasize on the choice of the boundary conditions in the RMF approach and superfluidity of the inner crust. Three kinds of boundary conditions are suggested. The properties of the W-S cells with the three kinds of boundary conditions are investigated. The neutron density distributions in the RMF and Hartree-Fock-Bogoliubov(HFB) models are compared.

2018 ◽  
Vol 98 (2) ◽  
Z.-X. Liu ◽  
C.-J. Xia ◽  
W.-L. Lu ◽  
Y.-X. Li ◽  
J. N. Hu ◽  

2012 ◽  
Vol 21 (08) ◽  
pp. 1250074 ◽  

Densities from relativistic mean field calculations are applied to construct the optical potential and, hence calculate the endpoint of the rapid proton capture (rp) process. Mass values are taken from a new phenomenological mass formula. Endpoints are calculated for different temperature-density profiles of various X-ray bursters. We find that the rp process can produce significant quantities of nuclei upto around mass 95. Our results differ from existing works to some extent.

1998 ◽  
Vol 57 (2) ◽  
pp. 857-865 ◽  
A. Delfino ◽  
Lizardo H. C. M. Nunes ◽  
J. S. Sá Martins

1999 ◽  
Vol 651 (2) ◽  
pp. 117-139 ◽  
S.K. Patra ◽  
Cheng-Li Wu ◽  
C.R. Praharaj ◽  
Raj K. Gupta

Universe ◽  
2019 ◽  
Vol 5 (10) ◽  
pp. 204 ◽  
Domenico Logoteta ◽  
Ignazio Bombaci

We discuss the constraints on the equation of state (EOS) of neutron star matter obtained by the data analysis of the neutron star-neutron star merger in the event GW170807. To this scope, we consider two recent microscopic EOS models computed starting from two-body and three-body nuclear interactions derived using chiral perturbation theory. For comparison, we also use three representative phenomenological EOS models derived within the relativistic mean field approach. For each model, we determine the β -stable EOS and then the corresponding neutron star structure by solving the equations of hydrostatic equilibrium in general relativity. In addition, we calculate the tidal deformability parameters for the two neutron stars and discuss the results of our calculations in connection with the constraints obtained from the gravitational wave signal in GW170817. We find that the tidal deformabilities and radii for the binary’s component neutron stars in GW170817, calculated using a recent microscopic EOS model proposed by the present authors, are in very good agreement with those derived by gravitational waves data.

1997 ◽  
Vol 357 (1) ◽  
pp. 33-38 ◽  
Andrzej Baran ◽  
Krzysztof Pomorski ◽  
Michał Warda

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