Alternative dark energy models: an overview
By J. A. S. Lima. 2004
133 citations recorded by the source corpus.
A large number of recent observational data strongly suggest that we live in a flat, accelerating Universe composed of » 1/3 of matter (baryonic + dark) and » 2/3 of an exotic component with large negative pressure, usually named Dark Energy or Quintessence. The basic set of experiments includes: observations from SNe Ia, CMB anisotropies, large scale structure, X-ray data from galaxy clusters, age estimates of globular clusters and old high redshift galaxies (OHRG’s). It is now widely believed that such results provide the remaining piece of information connecting the inflationary flatness prediction ( ›T = 1) with astronomical observations. From a theoretical viewpoint, they have also stimulated the current interest for more general models containing an extra component describing this unknown dark energy, and simultaneously accounting for the present accelerating stage of the Universe. In this review we present a simplified picture of the main results and discuss briefly some difficulties underlying the emerging dark energy paradigm.
Subfields: Artificial Intelligence, Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/5eee927383b3fb10e8ff500e94fa4cb30311cb3d
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Citations in the corpus
- Transition redshift: new kinematic constraints from supernovae (2008, background): “However, independent theoretical observational analyzes points to more general models whose basic ingredient is a negativepressure dark energy component (for review see, Padmanabhan 2003; Peebles & Ratra 2003; Lima 2004; Copeland et al. 2006).”
- Cosmological constraints on f(R) gravity theories within the Palatini approach (2005, result): “…2003, 2004a,b, 2005; Abdalla et al. 2005; Freese & Lewis 2002; Meng & Wang 2003; Dolgov & Kawasaki 2003; Shao et al. 2005; Gong et al. 2004; Lima 2004; Ahmed et al. 2004; Bento et al. 2002, 2003) have been proposed, and they can with some degree of success account for the observations (Lue…”
- Expansion History with Decaying Vacuum: A Complete Cosmological Scenario (2012, background): “The simplest type of DE corresponds to the cosmological constant (hereafter CC) (Weinberg 1989; Peebles & Ratra 2003; Padmanabhan 2003; Lima 2004).”