Coupled quintessence
A new component of the cosmic medium, a light scalar field or “quintessence,” has been proposed recently to explain cosmic acceleration with a dynamical cosmological constant. Such a field is expected to be coupled explicitly to ordinary matter, unless some unknown symmetry prevents it. I investigat...
Gespeichert in:
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
24 July 2000
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| In: |
Physical review. D, Particles, fields, gravitation, and cosmology
Year: 2000, Jahrgang: 62, Heft: 4 |
| ISSN: | 1550-2368 |
| DOI: | 10.1103/PhysRevD.62.043511 |
| Online-Zugang: | Verlag, Volltext: http://dx.doi.org/10.1103/PhysRevD.62.043511 Verlag, Volltext: https://link.aps.org/doi/10.1103/PhysRevD.62.043511 
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| Verfasserangaben: | Luca Amendola |
MARC
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| 520 | |a A new component of the cosmic medium, a light scalar field or “quintessence,” has been proposed recently to explain cosmic acceleration with a dynamical cosmological constant. Such a field is expected to be coupled explicitly to ordinary matter, unless some unknown symmetry prevents it. I investigate the cosmological consequences of a coupled quintessence (CQ) model, assuming an exponential potential and a linear coupling. This model is conformally equivalent to Brans-Dicke Lagrangians with any power-law potential. I evaluate the density perturbations on the cosmic microwave background and on the galaxy distribution at the present and derive bounds on the coupling constant from the comparison with observational data. A novel feature of CQ is that during the matter dominated era the scalar field has a finite and almost constant energy density. This epoch, denoted as φMDE, is a saddle point in the dynamical phase space. The φMDE is responsible of several differences with respect to uncoupled quintessence: the multipole spectrum of the microwave background is tilted at large angles, the acoustic peaks are shifted, their amplitude is changed, and the present 8 Mpc/h density variance is diminished. The present data constrain the dimensionless coupling constant to |β|<~0.1 assuming Ωm=0.3 and a primordial fluctuation slope ns=1. | ||
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