Abstract
Analyses of internal galaxy and cluster dynamics typically employ Newton’s law of gravity, which neglects the field self-interaction effects of General Relativity. This may be why dark matter seems necessary. The universe evolution, on the other hand, is treated with the full theory, General Relativity. However, the approximations of isotropy and homogeneity, normally used to derive and solve the universe evolution equations, effectively suppress General Relativity’s field self-interaction effects and this may introduce the need for dark energy. Calculations have shown that field self-interaction increases the binding of matter inside massive systems, which may account for galaxy and cluster dynamics without invoking dark matter. In turn, energy conservation dictates that the increased binding must be balanced by an effectively decreased gravitational interaction outside the massive system. In this article, such suppression is estimated and its consequence for the Universe’s evolution is discussed. Observations are reproduced without need for dark energy.
Highlights
General Relativity (GR)’s Lagrangian density is: LGR =det(gμν ) gμν Rμν, (1)where G is the Newton constant, gμν the metric and Rμν the Ricci tensor
What happens in the self-interaction framework can be sketched as follow: As DM (z) departs from 1, viz as gravity weakens globally, energy conservation demands that the global weakening is balanced locally by an increase of gravity within the structures themselves, speeding up their formation compared to a universe without selfinteraction
The Lagrangian of General Relativity contains field selfinteraction terms that become important for very massive systems
Summary
Where G is the Newton constant, gμν the metric and Rμν the Ricci tensor. The deviation of gμν from a constant reference metric ημν defines the gravity field, ψμν = gμν − ημν. [4,5] indicate that self-interaction increases sufficiently the gravitational binding of large massive systems such that no dark matter nor ad-hoc gravity/dynamical law modifications are needed to account for the galaxy missing mass problem. An important point for the present article is that the morphology of the massive structures in which gravity may be trapped determines how effective the trapping is: the less isotropic and homogeneous a system is, the larger the trapping is This implies a correlation between the missing mass of elliptical galaxies and their ellipticities. This was conjectured in Ref. [4] and the present article investigates this possibility
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