1994/07/27 by Franz E. Schunck, Eckehard W. Mielke · 40 citations
Mathematics · Physics and Astronomy · #Astrophysics #Black Holes and Theoretical Physics #Classical mechanics #Cosmology #Cosmology and Gravitation Theories #Dark energy #Deflation #Exact solutions in general relativity #Galaxies: Formation, Evolution, Phenomena #Geometry #Hubble's law #Inflation (cosmology) #Inflationary epoch #Mathematics #Metric (unit) #Metric expansion of space #Physics #Quantum mechanics #Scalar (mathematics) #Scalar field #Theoretical physics #Universe #astro-ph #gr-qc #hep-th
paper · pdf · doi:10.1103/physrevd.50.4794
published in Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields 50(8), 4794-4806 (American Physical Society) · 32 pages, REVTeX, 9 postscript figures (or hardcopy) available upon request, Cologne-thp-1994-H8
arxiv created 1994/07/27 · openalex publication_date 1994/10/15 · arxiv updated 2009/11/30 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
The mechanism of the initial inflation of the universe is based on graviationally coupled scalar fields \ensuremathφ. Various scenarios are distinguished by the choice of an effective self-interaction potential U(\ensuremathφ) which simulates a temporarily nonvanishing cosmological term. Using the Hubble expansion parameter H as a new ``time'' coordinate, we can formally derive the general Robertson-Walker metric for a spatially flat cosmos. Our new method provides a classification of allowed inflationary potentials and is broad enough to embody all known exact solutions involving one scalar field as special cases. Moreover, we present new inflationary and deflationary exact solutions and can easily predict the influence of the form of U(\ensuremathφ) on density perturbations.