2017/07/31 by S. A. Bonometto, Silvio A. Bonometto, Roberto Mainini
Physics and Astronomy · #Astrophysics #Cosmology and Gravitation Theories #Dark Matter and Cosmic Phenomena #Dark matter #Density contrast #Economics #Galaxies: Formation, Evolution, Phenomena #Galaxy #Momentum (technical analysis) #Physics #Statistical physics #Thermodynamics #Virial coefficient #Virial theorem #astro-ph.CO
paper · pdf · doi:10.3390/e19080398
published as Entropy, 2017, 19(8), 398 · 20 pages, 7 figures; updated to match the published version
openalex publication_date 2017/08/02 · arxiv created 2017/10/11 · arxiv updated 2017/10/12 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Strongly-Coupled Dark Energy plus Warm dark matter (SCDEW) cosmologies admit the stationary presence of ∼1% of coupled-DM and DE, since inflationary reheating. Coupled-DM fluctuations therefore grow up to non-linearity even in the early radiative expansion. Such early non-linear stages are modelized here through the evolution of a top-hat density enhancement, reaching an early virial balance when the coupled-DM density contrast is just 25–26, and the DM density enhancement is ∼10 % of the total density. During the time needed to settle in virial equilibrium, the virial balance conditions, however, continue to modify, so that “virialized” lumps undergo a complete evaporation. Here, we outline that DM particles processed by overdensities preserve a fraction of their virial momentum. Although fully non-relativistic, the resulting velocities (moderately) affect the fluctuation dynamics over greater scales, entering the horizon later on.