Speaker
Description
One of the problems in the modern cosmology is a so-called Hubble tension (HT), which is the difference between values of the present Hubble constant H0, measured by observation of the universe at redshift z ≤1, and the same value measured by observations of a distant universe by observations of CMB fluctuations corresponding to z ≌1100. We suggest that this Tension may be explained by deviation of the cosmological expansion from a standard 𝜦CDM model of a flat universe, due to the action of an additional variable component DEV during the post-recombination stage.
In order to maintain the almost constant DEV/DM energy density ratio during the whole time interval at $z < 1100$, it is necessary to allow the existence of a wide mass DM particle distribution.
