NUMERICAL METHODS FOR SOLVING THE RELATIVISTIC OPPENHEIMER–VOLKOFF EQUATIONS

P. J. Papasotiriou (), V. S. Geroyannis () and S. A. Sanidas
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P. J. Papasotiriou: Department of Materials Science, University of Patras, Greece
V. S. Geroyannis: Astronomy Laboratory, Department of Physics, University of Patras, Greece
S. A. Sanidas: Astronomy Laboratory, Department of Physics, University of Patras, Greece

International Journal of Modern Physics C (IJMPC), 2007, vol. 18, issue 11, 1735-1746

Abstract: In this paper, three methods for computing non-rotating neutron star models are discussed. The relativistic Oppenheimer–Volkoff (OV) equations of hydrostatic equilibrium are solved using (a) the well-known variable step method, (b) a method based on a modified form of the OV equations, where the thermodynamic enthalpy function is the independent variable, and (c) a new straightforward method, based on the ODEPACK Fortran package for solving systems of differential equations. We present results concerning several equations of state and conclusions concerning the applicability of each method.

Keywords: Equations of state; methods: numerical; stars: neutron; 02.60.Lj; 02.60.-x; 04.25.Dm; 97.60.Jd; 47.75.+f (search for similar items in EconPapers)
Date: 2007
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DOI: 10.1142/S0129183107011704

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