skip to main content
OSTI.GOV title logo U.S. Department of Energy
Office of Scientific and Technical Information

Title: Relativistic mean field calculations in neutron-rich nuclei

Abstract

Relativistic mean field calculations have been employed to study neutron rich nuclei. The Lagrange's equations have been solved in the co-ordinate space. The effect of the continuum has been effectively taken into account through the method of resonant continuum. It is found that BCS approximation performs as well as a more involved Relativistic Continuum Hartree Bogoliubov approach. Calculations reveal the possibility of modification of magic numbers in neutron rich nuclei. Calculation for low energy proton scattering cross sections shows that the present approach reproduces the density in very light neutron rich nuclei.

Authors:
;  [1];  [2]
  1. Department of Physics, University of Calcutta, 92 Acharya Prafulla Chandra Road, Kolkata 700 009 (India)
  2. Saha Institute of Nuclear Physics, Block AF, Sector 1, Kolkata- 700 064 (India)
Publication Date:
OSTI Identifier:
22308441
Resource Type:
Journal Article
Resource Relation:
Journal Name: AIP Conference Proceedings; Journal Volume: 1609; Journal Issue: 1; Conference: FIG12: International conference on frontiers in gamma-ray spectroscopy 2012, New Delhi (India), 5-7 Mar 2012; Other Information: (c) 2014 AIP Publishing LLC; Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
71 CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS; CROSS SECTIONS; LAGRANGE EQUATIONS; MAGIC NUCLEI; MEAN-FIELD THEORY; NEUTRON-RICH ISOTOPES; RELATIVISTIC RANGE; SCATTERING

Citation Formats

Gangopadhyay, G., Bhattacharya, Madhubrata, and Roy, Subinit. Relativistic mean field calculations in neutron-rich nuclei. United States: N. p., 2014. Web. doi:10.1063/1.4893254.
Gangopadhyay, G., Bhattacharya, Madhubrata, & Roy, Subinit. Relativistic mean field calculations in neutron-rich nuclei. United States. doi:10.1063/1.4893254.
Gangopadhyay, G., Bhattacharya, Madhubrata, and Roy, Subinit. 2014. "Relativistic mean field calculations in neutron-rich nuclei". United States. doi:10.1063/1.4893254.
@article{osti_22308441,
title = {Relativistic mean field calculations in neutron-rich nuclei},
author = {Gangopadhyay, G. and Bhattacharya, Madhubrata and Roy, Subinit},
abstractNote = {Relativistic mean field calculations have been employed to study neutron rich nuclei. The Lagrange's equations have been solved in the co-ordinate space. The effect of the continuum has been effectively taken into account through the method of resonant continuum. It is found that BCS approximation performs as well as a more involved Relativistic Continuum Hartree Bogoliubov approach. Calculations reveal the possibility of modification of magic numbers in neutron rich nuclei. Calculation for low energy proton scattering cross sections shows that the present approach reproduces the density in very light neutron rich nuclei.},
doi = {10.1063/1.4893254},
journal = {AIP Conference Proceedings},
number = 1,
volume = 1609,
place = {United States},
year = 2014,
month = 8
}
  • Properties of symmetric nuclear matter and neutron-rich matter predicted by effective field based relativistic mean field parameter sets are compared to those presented in a recent analysis of nuclear giant monopole resonance and isospin diffusion data and a study of the neutron skin of finite nuclei, as well as some selected observational data of neutron stars. Motivated by the fact that none of the published parameter sets of this model is simultaneously consistent with all previously mentioned constraints, an improvement not only in the isovector sector but also in isoscalar sector of this model is proposed. The properties of symmetricmore » nuclear matter and neutron-rich matter, as well as some basic properties of static neutron stars predicted by the proposed parameter set (G2**), are discussed.« less
  • Relativistic mean-field (RMF) theory is applied to investigate the properties of the radioactive neutron-rich doubly magic nucleus {sup 132}Sn and the corresponding isotopes and isotones. The two-neutron and two-proton separation energies are well reproduced by the RMF theory. In particular, the RMF results agree with the experimental single-particle spectrum in {sup 132}Sn as well as the Nilsson spin-orbit parameter C and orbit-orbit parameter D thus extracted, but remarkably differ from the traditional Nilsson parameters. Furthermore, the present results provide a guideline for the isospin dependence of the Nilsson parameters.
  • We have studied the present theoretical understanding of size of neutron, proton, matter, and charge distributions in spherical nuclei. The ground-state nuclear radii have been evaluated in the framework of the relativistic mean-field approach within the Hartree approximation. A comparison has been done with the radii obtained with the nonrelativistic density-dependent Skyrme interactions. It is pointed out that with an increase in isospin of nuclei, the neutron rms radii in the relativistic mean-field approach are larger than both the empirical data and the predictions of the Skyrme mean field.
  • We study the properties of nuclei in the inner crusts of neutron stars based on the Boguta-Bodmer nonlinear model in the relativistic mean-field theory. We carefully determine the surface diffuseness of the nuclei as the density of matter increases. The imaginary time step method is used to solve the Euler-Lagrange equation derived from the variational principle applied to the semiclassical energy density. It is shown that with increasing density, the spherical nuclei become more neutron rich and eventually merge to form a uniform liquid of neutrons, protons, and electrons. We find that the smaller the value of the incompressibility K,more » the lower the density at which the phase transition to uniform matter occurs. The relativistic extended Thomas-Fermi method is generalized to investigate nonspherical nuclei. Our results show that the spherical nucleus phase is the only equilibrium state in the inner crusts of neutron stars. {copyright} {ital 1997} {ital The American Physical Society}« less
  • Cited by 26