2019/04/17 by Matteo Tuveri, Tuveri, Matteo, Mariano Cadoni +1
Physics and Astronomy · #Astrophysics #Black Holes and Theoretical Physics #Classical mechanics #Cosmological constant #Cosmology #Cosmology and Gravitation Theories #Cosmology and Nongalactic Astrophysics (astro-ph.CO) #Dark energy #Dark matter #De Sitter universe #Einstein field equations #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Galaxy rotation curve #General Relativity and Quantum Cosmology (gr-qc) #General relativity #High Energy Physics - Theory (hep-th) #Modified Newtonian dynamics #Physics #Theoretical physics #Universe #astro-ph.CO #gr-qc #hep-th
paper · pdf · doi:10.48550/arxiv.1904.08209
5 pages, no figures, letter
arxiv created 2019/04/17 · openalex publication_date 2019/04/17 · arxiv updated 2019/04/18 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We derive the radial acceleration of stars in galaxies by using basic features of thermodynamics, statistical mechanics and general relativity. We assume that the "dark" component of the radial acceleration is originated from the reaction of dark energy to the presence of baryonic matter. It can be also explained as the macroscopic manifestation of a huge number of extremely soft bosonic excitations of the dark energy medium with wavelength larger than the size of the cosmological horizon, in thermal equilibrium with de Sitter spacetime. Our formula agrees with the phenomenological relation proposed by McGaugh et al. which, in turns, fits a large amount of observational data and with the MOND theory. We also show that our formula appears as the weak field limit of Einstein's general relativity sourced by an anisotropic fluid.