Nuclear shape transition at finite temperature in a relativistic mean field approach

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.

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Octupole degree of freedom for nuclei near152Sm in a reflection-asymmetric relativistic mean-field approach

Journal of Physics Conference Series ◽

10.1088/1742-6596/312/9/092066 ◽

2011 ◽

Vol 312 (9) ◽

pp. 092066

Author(s):

W Zhang ◽

Z P Li ◽

S Q Zhang ◽

J Meng

Keyword(s):

Mean Field ◽

Degree Of Freedom ◽

Field Approach ◽

Relativistic Mean Field

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Relativistic mean-field approach for Λ,Ξ , and Σ hypernuclei

Physical Review C ◽

10.1103/physrevc.98.024316 ◽

2018 ◽

Vol 98 (2) ◽

Cited By ~ 11

Author(s):

Z.-X. Liu ◽

C.-J. Xia ◽

W.-L. Lu ◽

Y.-X. Li ◽

J. N. Hu ◽

...

Keyword(s):

Mean Field ◽

Field Approach ◽

Relativistic Mean Field

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FINITE TEMPERATURE EQUATIONS OF STATE FOR MIXED STARS

International Journal of Modern Physics D ◽

10.1142/s0218271804005389 ◽

2004 ◽

Vol 13 (07) ◽

pp. 1249-1253

Author(s):

DÉBORA P. MENEZES ◽

C. PROVIDÊNCIA

Keyword(s):

Field Theory ◽

Neutron Stars ◽

Quark Matter ◽

Finite Temperature ◽

Equations Of State ◽

Mean Field Theory ◽

Mean Field ◽

Relativistic Mean Field Theory ◽

Relativistic Mean Field

We investigate the properties of mixed stars formed by hadronic and quark matter in β-equilibrium described by appropriate equations of state (EOS) in the framework of relativistic mean-field theory. The calculations were performed for T=0 and for finite temperatures and also for fixed entropies with and without neutrino trapping in order to describe neutron and proto-neutron stars. The star properties are discussed. Maximum allowed masses for proto-neutron stars are much larger when neutrino trapping is imposed.

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ENDPOINT OF rp PROCESS USING RELATIVISTIC MEAN FIELD APPROACH AND A NEW MASS FORMULA

International Journal of Modern Physics E ◽

10.1142/s0218301312500747 ◽

2012 ◽

Vol 21 (08) ◽

pp. 1250074 ◽

Cited By ~ 6

Author(s):

CHIRASHREE LAHIRI ◽

G. GANGOPADHYAY

Keyword(s):

Mass Formula ◽

Optical Potential ◽

Mean Field ◽

Proton Capture ◽

Density Profiles ◽

X Ray ◽

Field Approach ◽

Relativistic Mean Field ◽

Rapid Proton ◽

Rp Process

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.

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