How to determine an effective potential for a variable cosmological term

1998/10/27 by A. A. Starobinsky · 16 citations
Physics and Astronomy · #Cosmology and Gravitation Theories #Pulsars and Gravitational Waves Research #Relativity and Gravitational Theory #astro-ph #gr-qc

paper · pdf · doi:10.1134/1.567941

published as JETP Lett. 68 (1998) 757-763; Pisma Zh.Eksp.Teor.Fiz. 68 (1998) 721-726 · Latex, 7 pages, JETP Lett., in press, 1998

arxiv created 1998/10/27 · openalex publication_date 1998/11/01 · arxiv updated 2009/11/30 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/31

Abstract

It is shown that if a variable cosmological term in the present Universe is described by a scalar field with minimal coupling to gravity and with some phenomenological self-interaction potential V (ϕ), then this potential can be unambiguously determined from the following observational data: either from the behavior of density perturbations in dustlike matter component as a function of redshift (given the Hubble constant additionally), or from the luminosity distance as a function of redshift (given the present density of dustlike matter in terms of the critical value).

Citations

• Cosmological consequences of a rolling homogeneous scalar field

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