Inflation and quintessence with nonminimal coupling
By Valerio Faraoni. 2000
272 citations recorded by the source corpus.
The nonminimal coupling (NMC) of the scalar field to the Ricci curvature is unavoidable in many cosmological scenarios. Inflation and quintessence models based on nonminimally coupled scalar fields are studied, with particular attention to the balance between the scalar potential and the NMC term ξRφ2/2 in the action. NMC makes acceleration of the universe harder to achieve for the usual potentials, but it is beneficial in obtaining cosmic acceleration with unusual potentials. The slow-roll approximation with NMC, conformal transformation techniques, and other aspects of the physics of NMC are clarified. ©2000 The American Physical Society.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/ab7d7d1b968e378c7affea754bfc9314895ba2b9
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In Astronomy and Astrophysics
- Lavinia Heisenberg
- S. Tsujikawa
- Tomi Koivisto
- H. Hoekstra
- Emmanuel N. Saridakis
- Thomas D. Kitching
- Catherine Heymans
- Pedro G. Ferreira
In Nuclear and High Energy Physics
- Lavinia Heisenberg
- S. Tsujikawa
- Tomi Koivisto
- Emmanuel N. Saridakis
- D. Mota
- Claudia de Rham
- Pedro G. Ferreira
- C. Skordis
Citations in the corpus
- Cosmology and Fundamental Physics with the Euclid Satellite (2012, background): “Scalar–tensor theories (Wetterich 1988; Hwang 1990a, b; Damour et al. 1990; Casas et al. 1991, 1992; Wetterich 1995; Uzan 1999; Perrotta et al. 2000; Faraoni 2000; Boisseau et al. 2000; Riazuelo and Uzan 2002; Perrotta and Baccigalupi 2002; Schimd et al. 2005; Matarrese et al. 2004; Pettorino et al.”
- Observational constraints on teleparallel dark energy (2011, background): “The first is to modify the content of the universe by introducing the dark energy sector, which can be based on a canonical scalar field (quintessence) [6–22], a phantom field [23–28], or on the combination of both these fields in a unified scenario called quintom [29–35] (see [36] for a review).”
- The Cosmological Constant and Dark Energy (2002, background): “111 See Uzan (1999), Chiba (1999), Amendola (1999, 2000), Perrotta, Baccigalupi, and Matarrese (2000), Bartolo and Pietroni (2000), Bertolami and Martins (2000), Fujii (2000), Faraoni (2000), Baccigalupi et al. (2000), Chen, Scherrer, and Steigman (2001), and references therein.”