Hubble tension and absolute constraints on the local Hubble parameter

Abstract

It is shown, from the two independent approaches of McCrea-Milne and of Zeldovich, that one can fully recover the set equations corresponding to the relativistic equations of the expanding universe of Friedmann-Lemaitre-Robertson-Walker geometry. Although similar, the Newtonian and relativistic set of equations have a principal difference in the content and hence define two flows, local and global ones, thus naturally exposing the Hubble tension at the presence of the cosmological constant Λ. From this, we obtain absolute constraints on the lower and upper values for the local Hubble parameter, √(Λc2/3) ≃ 56.2 and √(Λc2) ≃ 97.3 (km s−1 Mpc−1), respectively. The link to the so-called maximum force–tension issue in cosmological models is revealed.

Gravitational waves as waveguides

“…That formalism appears to be efficient in the studying the properties of the Cosmic Microwave Background (CMB), Cold Spot, photon propagation through cosmic voids [16,17,18,19], linked to the Hubble tension, e.g. [20,21]. We show that, within certain conditions, the photons if initially aligned with the gravitational waves, will continue to propagate keeping their alignment, i.e.…”

From maximum force to physics in 9 lines and towards relativistic quantum gravity

“…The maximum force limit is not the only option to describe general relativity. Other limit quantities that combine c and G, such as maximum power c 5 /4G [11,17,21,25,36,37,[40][41][42][43],…”

The cosmological constant vs adiabatic invariance

“…The weak-field modification of GR involving the cosmological constant is among the suggested approaches to the Hubble tension problem [12,13]. It is based on a theorem proved in [14] that the general function for the force satisfying the identity of the sphere's and point mass's gravity field has the form…”

“…In this form the cosmological constant Λ enters the weak-field GR, and enables to describe the dynamics of groups and clusters of galaxies, as well as the flow of the Local Supercluster [17]. Namely, it appears that two Hubble flows can be distinguished, the local one described by the weak-field GR, and the global one described by Friedmannian equations [12,13]. This is linked also with the problem of the formation of the cosmic web [18] and the voids (e.g.…”