2004/03/03 by Eduardo Guendelman, E. I. Guendelman, Guendelman, E. I. +3
Computer Science · Physics and Astronomy · #Astrophysics (astro-ph) #Computational Physics and Python Applications #Cosmology and Gravitation Theories #FOS: Physical sciences #General Relativity and Quantum Cosmology (gr-qc) #High Energy Physics - Phenomenology (hep-ph) #High Energy Physics - Theory (hep-th) #Relativity and Gravitational Theory #astro-ph #gr-qc #hep-ph #hep-th
paper · pdf · doi:10.48550/arxiv.gr-qc/0403017
5 pages; presented to the proceedings of the Tenth Marcel Grossmann Meeting
arxiv created 2004/03/03 · openalex publication_date 2004/03/03 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Scale invariance is considered in the context of a gravitational theory where the action, in the first order formalism, is of the form S = ∫ L1 Φd4x + ∫ L2√(-g)d4x where Φis a density built out of degrees of freedom independent of the metric. For global scale invariance, a "dilaton" ϕhas to be introduced, with non-trivial potentials V(ϕ)=f1eαϕ in L1 and U(ϕ) = f2e2αϕ in L2. In the effective Einstein frame, this leads to a non-trivial ϕpotential (of the Morse type) which has a flat region with energy density f12/4f2 as ϕ→∞. The addition of an R2 term produces an effective potential with two connected flat regions: one of the Planck scale, that can be responsible for early inflation, and another for the description of the present universe.