Newtonian view of general relativistic stars

The European Physical Journal C

H. E. S. Velten¹  J. C. Fabris¹  A. M. Oliveira²  I. G. Salako³ 

[1] Departamento de Física, Universidade Federal do Espírito Santo (UFES), Vitória, Brazil;Grupo de Ciências Ambientais e Recursos Naturais, Instituto Federal do Espírito Santo (IFES), Guarapari, Brazil;Institut de Mathématiques et de Sciences Physiques (IMSP), Porto-Novo, Bénin;

关键词: Neutron Star;    Maximum Mass;    Friedmann Equation;    Hydrostatic Equilibrium;    Cosmological Solution;   

DOI  :  10.1140/epjc/s10052-014-3170-2

来源: Springer

【 摘 要 】

Although general relativistic cosmological solutions, even in the presence of pressure, can be mimicked by using neo-Newtonian hydrodynamics, it is not clear whether there exists the same Newtonian correspondence for spherical static configurations. General relativity solutions for stars are known as the Tolman–Oppenheimer–Volkoff (TOV) equations. On the other hand, the Newtonian description does not take into account the total pressure effects and therefore cannot be used in strong field regimes. We discuss how to incorporate pressure in the stellar equilibrium equations within the neo-Newtonian framework. We compare the Newtonian, neo-Newtonian, and the full relativistic theory by solving the equilibrium equations for both three approaches and calculating the mass–radius diagrams for some simple neutron stars’ equations of state.

【 授权许可】

CC BY