NUMERICAL METHODS FOR SOLVING THE RELATIVISTIC OPPENHEIMER–VOLKOFF EQUATIONS

DOI10.1142/S0129183107011704zbMath1170.83399MaRDI QIDQ3500231

S. A. Sanidas, P. J. Papasotiriou, V. S. Geroyannis

Publication date: 3 June 2008

Published in: International Journal of Modern Physics C (Search for Journal in Brave)

zbMATH Keywords

Fortran packagevariable step methodnon-rotating neutron star modelsrelativistic Oppenheimer-Volkoff equations of hydrostatic equilibrium

Mathematics Subject Classification ID

Numerical methods for initial value problems involving ordinary differential equations (65L05) Macroscopic interaction of the gravitational field with matter (hydrodynamics, etc.) (83C55) PDEs in connection with relativity and gravitational theory (35Q75) Galactic and stellar dynamics (85A05)

Related Items (2)

NUMERICAL TREATMENT OF ROTATING NEUTRON STARS SIMULATED BY GENERAL-RELATIVISTIC POLYTROPIC MODELS: A COMPLEX-PLANE STRATEGY ⋮ NUMERICAL TREATMENT OF HARTLE'S PERTURBATION METHOD FOR DIFFERENTIALLY ROTATING NEUTRON STARS SIMULATED BY GENERAL-RELATIVISTIC POLYTROPIC MODELS

Uses Software

• Unnamed Item
• ODEPACK
• LORENE

Cites Work

• Phase transitions in compact stars
• Automatic Selection of Methods for Solving Stiff and Nonstiff Systems of Ordinary Differential Equations
• A SCILAB PROGRAM FOR COMPUTING GENERAL-RELATIVISTIC MODELS OF ROTATING NEUTRON STARS BY IMPLEMENTING HARTLE'S PERTURBATION METHOD

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