TITLE:
The Equation of State of Nuclear Matter and Neutron Stars Properties
AUTHORS:
Khaled S. A. Hassaneen
KEYWORDS:
Symmetric Nuclear Matter, Equation of State, Three-Body Force, Pressure, Incompressibility, Neutron Star Properties
JOURNAL NAME:
Journal of Modern Physics,
Vol.5 No.16,
October
30,
2014
ABSTRACT: The
equation of state (EOS) of symmetric nuclear and pure neutron matter has been
investigated extensively by adopting the non-relativistic
Brueckner-Hartree-Fock (BHF). For more comparison, the extended BHF approaches
using the self-consistent Green’s function approach or by including a
three-body force will be done. The EOS will be studied for different approaches
at zero temperature. We can calculate the total mass and radius of neutron
stars using various equations of state. A comparison with relativistic BHF
calculations will be done. Relativistic effects are known to be important at
high densities, giving an increased repulsion. This leads to a stiffer EOS
compared to the EOS derived with a non-relativistic approach.