Systematics of nuclear matter and finite nuclei properties in a non-linear relativistic mean field approach

1984 ◽  
Vol 422 (3) ◽  
pp. 541-581 ◽  
Author(s):  
A. Bouyssy ◽  
S. Marcos ◽  
Pham Van Thieu
Keyword(s):  
Nuclear Matter ◽  
Mean Field ◽  
Field Approach ◽  
Relativistic Mean Field ◽  
Non Linear ◽  
Finite Nuclei

ELECTROMAGNETIC AND ISOVECTOR TERMS IN STANDARD RELATIVISTIC MEAN FIELD MODEL

2011 ◽  
Vol 20 (09) ◽  
pp. 1983-2010 ◽  
Author(s):  
A. SULAKSONO
Keyword(s):  
Nuclear Matter ◽  
Field Model ◽  
Local Density ◽  
Mean Field ◽  
Binding Energies ◽  
Particle Spectrum ◽  
Mean Field Model ◽  
Density Dependent ◽  
Relativistic Mean Field ◽  
Finite Nuclei

The effects of auxiliary contribution in forms of electromagnetic tensors and relativistic electromagnetic exchange in local density approximation as well as δ meson and isovector density-dependent nonlinear terms in standard relativistic mean field model constrained by nuclear matter stability criteria in some selected finite nuclei and nuclear matter properties are studied. It is found that in the case of finite nuclei, the electromagnetic tensors play the most dominant part compared to other auxiliary terms. Due to the presence of electromagnetic tensors, the binding energies prediction of the model can be improved quite significantly. However, these terms do not yield demanded effects for rms radii prediction. In the case of nuclear matter properties, the isovector density-dependent nonlinear term plays the most crucial role in providing predictions which are quite compatible with experimental constraints. We have also shown these auxiliary contributions are indeed unable to improve the single particle spectrum results of the model.

ISOVECTOR COMPONENTS OF LIGHT SCALAR MESON AND NUCLEAR MATTER PROPERTIES

2007 ◽  
Vol 16 (09) ◽  
pp. 2867-2871 ◽  
Author(s):  
C. A. Z. VASCONCELLOS ◽  
E. LÜTZ ◽  
M. RAZEIRA ◽  
B. E. J. BODMANN ◽  
M. DILLIG ◽  
...  
Keyword(s):  
Nuclear Matter ◽  
Scalar Meson ◽  
Mean Field ◽  
Symmetry Transformation ◽  
Hadronic Matter ◽  
Meson Field ◽  
Field Approach ◽  
Relativistic Mean Field ◽  
Light Scalar ◽  
Scalar Meson Field

We have predicted (contribution to this issue) an isovector component of the light scalar meson sector by using the chiral symmetry transformation formalism. On the basis of this result, we study dense hadronic matter in a generalized relativistic mean field approach with σ, ω and ρ mesons as well as nonlinear self-couplings of the I = 1 component of a light scalar meson field and compare its predictions for neutron star properties with results from different models for nuclear matter found in the literature.

scholarly journals Spinodal instabilities in nuclear matter in a stochastic relativistic mean-field approach

2009 ◽  
Vol 80 (3) ◽  
Author(s):  
S. Ayik ◽  
O. Yilmaz ◽  
N. Er ◽  
A. Gokalp ◽  
P. Ring
Keyword(s):  
Nuclear Matter ◽  
Mean Field ◽  
Field Approach ◽  
Relativistic Mean Field

scholarly journals Effects of NN potentials on p Nuclides in the A ∼100–120 region

2016 ◽  
Vol 25 (02) ◽  
pp. 1650015 ◽  
Author(s):  
C. Lahiri ◽  
S. K. Biswal ◽  
S. K. Patra
Keyword(s):  
Experimental Data ◽  
Nuclear Matter ◽  
Mean Field ◽  
Reaction Rates ◽  
Mass Region ◽  
Low Energy ◽  
Field Approach ◽  
Relativistic Mean Field ◽  
Energy Proton ◽  
Energy Formula

Microscopic optical potentials for low-energy proton reactions have been obtained by folding density dependent M3Y (DDM3Y) interaction derived from nuclear matter calculation with densities from mean field approach to study astrophysically important proton rich nuclei in mass 100–120 region. We compare [Formula: see text] factors for low-energy [Formula: see text] reactions with available experimental data and further calculate astrophysical reaction rates for [Formula: see text] and [Formula: see text] reactions. Again, we choose some nonlinear R3Y (NR3Y) interactions from relativistic mean field (RMF) calculation and folded them with corresponding RMF densities to reproduce experimental [Formula: see text]-factor values in this mass region. Finally, the effect of nonlinearity on our result is discussed.

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