The Equation of State of Nuclear Matter and Neutron Stars Properties

Khaled S. A. Hassaneen^1,2*

¹PhysicsDepartment, Faculty of Science, Taif University, Taif, KSA.
²Physics Department, Faculty of Science, Sohag University, Sohag, Egypt.

DOI: 10.4236/jmp.2014.516171                

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.

Keywords

Symmetric Nuclear Matter, Equation of State, Three-Body Force, Pressure, Incompressibility, Neutron Star Properties

Conflicts of Interest

The authors declare no conflicts of interest.

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