2007/06/30 by Brendan Z. Foster, Brendan Foster · 1 citation
Mathematics · Physics and Astronomy · #Aether #Black Holes and Theoretical Physics #Classical mechanics #Cosmology and Gravitation Theories #Dimensionless quantity #Effective field theory #Einstein #Equations of motion #Field (mathematics) #General relativity #Mathematics #Physics #Pulsar #Pulsars and Gravitational Waves Research #Quantum mechanics #Theoretical physics #gr-qc
paper · pdf · doi:10.1103/physrevd.76.084033
published as Phys.Rev.D76:084033,2007 · 23 pages, 1 figure; v2: fixed error in Eqn. (70) and resulting bounds on c's
openalex publication_date 2007/10/25 · arxiv created 2008/09/23 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
``Einstein--aether'' theory is a generally covariant theory of gravity containing a dynamical preferred frame. This article continues an examination of effects on the motion of binary pulsar systems in this theory, by incorporating effects due to strong fields in the vicinity of neutron star pulsars. These effects are included through an effective approach, by treating the compact bodies as point particles with nonstandard, velocity dependent interactions parametrized by dimensionless sensitivities. Effective post-Newtonian equations of motion for the bodies and the radiation damping rate are determined. More work is needed to calculate values of the sensitivities for a given fluid source; therefore, precise constraints on the theory's coupling constants cannot yet be stated. It is shown, however, that strong field effects will be negligible given current observational uncertainties if the dimensionless couplings are less than roughly 0.1 and two conditions that match the PPN parameters to those of pure general relativity are imposed. In this case, weak field results suffice. There then exists a one-parameter family of Einstein--aether theories with ``small-enough'' couplings that passes all current observational tests. No conclusion can be reached for larger couplings until the sensitivities for a given source can be calculated.