Nuclear matter density effects in monopole transitions

1986 ◽  
Vol 33 (1) ◽  
pp. 40-49 ◽  
Author(s):  
M. Pignanelli ◽  
S. Micheletti ◽  
R. De Leo ◽  
S. Brandenburg ◽  
M. N. Harakeh
Keyword(s):  
Nuclear Matter ◽  
Matter Density ◽  
Nuclear Matter Density ◽  
Density Effects

Recent Results from Nuclear Lattice Simulations

2007 ◽  
Vol 22 (07n10) ◽  
pp. 555-564
Author(s):  
DEAN LEE
Keyword(s):  
Field Theory ◽  
Nuclear Matter ◽  
Effective Field Theory ◽  
Recent Progress ◽  
Effective Field ◽  
Matter Density ◽  
Neutron Matter ◽  
Chiral Effective Field Theory ◽  
Nuclear Matter Density ◽  
Work Done

We discuss recent progress in the study of nuclear and neutron matter by combining chiral effective field theory with non-perturbative lattice methods. We present results for hot neutron matter at temperatures 20 to 40 MeV and densities below twice nuclear matter density. This proceedings article is a summary of results from work done in collaboration with Bugra Borasoy and Thomas Schaefer1.

scholarly journals Quasi-elastic processes of the48Ca + 120Sn system and the48Ca nuclear matter density

2013 ◽  
Vol 88 (4) ◽  
Author(s):  
E. Crema ◽  
M. A. G. Alvarez ◽  
N. H. Medina ◽  
L. R. Gasques ◽  
J. F. P. Huiza ◽  
...  
Keyword(s):  
Nuclear Matter ◽  
Matter Density ◽  
Nuclear Matter Density ◽  
Elastic Processes

scholarly journals EQUILIBRIUM CONFIGURATIONS FOR QUARK–DIQUARK STARS AND THE PROBLEM OF HER X-1 MASS

1998 ◽  
Vol 07 (01) ◽  
pp. 19-27 ◽  
Author(s):  
J. E. HORVATH ◽  
J. A. DE FREITAS PACHECO
Keyword(s):  
Equation Of State ◽  
Physical Properties ◽  
Nuclear Matter ◽  
Stable State ◽  
Baryon Density ◽  
Matter Density ◽  
X Ray ◽  
Nuclear Matter Density ◽  
Equilibrium Configurations ◽  
Stellar Models

We report new calculations of the physical properties of a quark–diquark plasma. A vacuum contribution is taken into account and is responsible for the appearance of a stable state at zero pressure and at a baryon density of about 2.2 times the nuclear matter density in this model. The resulting equation of state was used to integrate numerically the Tolman–Oppenheimer–Volkoff equations. The mass-radius relationship has been derived from a series of equilibrium configurations constituted by a mixture of quarks and diquarks. These stellar models, which are representative of a whole class, may be helpful to understand the possible compactness of the X-ray source Her X-1 and related objects.

FINITE TEMPERATURE NUCLEAR MATTER IN THE RELATIVISTIC MEAN FIELD THEORY

2007 ◽  
Vol 16 (02n03) ◽  
pp. 297-302 ◽  
Author(s):  
TOMAZ PASSAMANI ◽  
MARIA LUIZA CESCATO
Keyword(s):  
Field Theory ◽  
Low Temperature ◽  
Nuclear Matter ◽  
Finite Temperature ◽  
Mean Field Theory ◽  
Mean Field ◽  
Matter Density ◽  
Relativistic Mean Field Theory ◽  
Relativistic Mean Field ◽  
Nuclear Matter Density

The nuclear matter density at finite temperature was evaluated analytically in the relativistic mean field theory using Sommerfeld approximation at low temperature. These analytical results are interesting since they allow a more transparent analysis of the contributions of the involved parameters.

A FUZZY BAG MODEL FOR NUCLEAR MATTER: A PRELIMINARY APPROACH

2010 ◽  
Vol 19 (08n10) ◽  
pp. 1593-1597 ◽  
Author(s):  
A. S. S. ROCHA ◽  
C. A. Z. VASCONCELLOS ◽  
F. FERNÁNDEZ
Keyword(s):  
Nuclear Matter ◽  
Internal Energy ◽  
Energy Function ◽  
Fermi Gas ◽  
Matter Density ◽  
Hydrostatic Equilibrium ◽  
Free Term ◽  
Bag Model ◽  
Nuclear Matter Density ◽  
Free Fermi

In this work we develop an effective formalism for nuclear matter based on the fuzzy bag model. The main objective of our study is to discuss the feasibility of using the fuzzy bag model to describe nuclear matter properties. The physical system is described in our approach by an internal energy function, which has a free term, corresponding to a free Fermi gas, and an interacting one. In the interacting part, pion exchange is taken into account via an effective potential. To avoid superposition of nucleons, we introduce an exclusion volume à la Van der Waals. The internal energy function depends on the nuclear matter density and also on a parameter which will determine the expected volume of a nucleon in matter. We then obtain results for the binding energy per nucleon for the symmetric nuclear matter and for neutron matter, as well as the equation of state within this model. We then determine the mass of neutron stars in hydrostatic equilibrium, using the TOV equations. In spite of utilizing a treatment that is still very preliminary, our results show the feasibility of using this treatment to describe nuclear matter properties.

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