2011/04/30 by J. A. Rueda, Jorge A. Rueda, R. Ruffini +2 · 3 citations
Earth and Planetary Sciences · Physics and Astronomy · #Classical mechanics #Einstein #Electromagnetic field #General relativity #Gravitation #Gravitational field #High-pressure geophysics and materials #Isothermal process #Mathematical physics #Physics #Pulsars and Gravitational Waves Research #Quantum electrodynamics #Quantum mechanics #Quantum, superfluid, helium dynamics #astro-ph.SR #gr-qc #nucl-th
paper · pdf · doi:10.1016/j.nuclphysa.2011.09.005
published as Nuclear Physics A, Volume 872, Issue 1, 286-295 (2011) · To be published by Nuclear Physics A
arxiv created 2011/09/13 · openalex publication_date 2011/10/02 · arxiv updated 2012/06/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
The isothermal Tolman condition and the constancy of the Klein potentials originally expressed for the sole gravitational interaction in a single fluid are here generalized to the case of a three quantum fermion fluid duly taking into account the strong, electromagnetic, weak and gravitational interactions. The set of constitutive equations including the Einstein-Maxwell-Thomas-Fermi equations as well as the ones corresponding to the strong interaction description are here presented in the most general relativistic isothermal case. This treatment represents an essential step to correctly formulate a self-consistent relativistic field theoretical approach of neutron stars.