New cosmological tracker solution for quintessence

By L. Arturo Ureña‐López, T. Matos. 2000

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In this paper we propose a quintessence model with the potential $V(\ensuremath{\Phi}{)=V}_{0}[\mathrm{sinh}(\ensuremath{\alpha}\sqrt{{\ensuremath{\kappa}}_{0}}\ensuremath{\Delta}\ensuremath{\Phi}){]}^{\ensuremath{\beta}}$ with $\ensuremath{\beta}l0,$ whose asymptotic behavior corresponds to an inverse power-law potential at early times and to an exponential one at late times. We demonstrate that this is a tracker solution and that it could have driven the Universe into its current inflationary stage. The exact solutions and the description for a complete evolution of the Universe are also given. We compare such a model with current cosmological observations.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/d307af6ea7e048d1b47315119098a165de6415f6

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Citations in the corpus

Is there supernova evidence for dark energy metamorphosis (2003, background): “Aside from the cosmological constant (w = −1), the topological defect models alluded to earlier and the sine-hyperbolic scalar field potential (Sahni & Starobinsky 2000; Urena-Lopez & Matos 2000; Sahni et al. 2003) no viable DE models exist with the property w = constant.”
Cosmological parameters from supernova observations: A critical comparison of three data sets (2003, background): “…which evolves with time (Ratra & Peebles 1988; Wetterich 1988; Ferreira & Joyce 1998; Frieman et al. 1995; Brax & Martin 1999; Brax & Martin 2000; Urena-Lopez & Matos 2000; Barreiro, Copeland, & Nunes 2000; Send offprint requests to: T. Roy Choudhury, e-mail:chou@sissa.it Zlatev, Wang, &…”
Observational constraints on teleparallel dark energy (2011, methodology): “ike component (CDM and baryons), dark energy with an exactly constant wDE > −1 is possible for the inverse hyperbolic sine potential in some power as was ﬁrst independently shown in Refs. [90] and [91]. 4 Conclusions In the present work we have used observational data to impose constraints on the”
Exploring the expanding Universe and dark energy using the statefinder diagnostic (2003, background): “Quiessence in a FRW universe can also be produced by a scalar field (quintessence) which has the potential V (φ) ∝ sinh −2(1+w) w (Cφ + D), with appropriately chosen values of C and D (see Sahni & Starobinsky 2000; Urena-Lopez & Matos 2000).”
WMAP constraints on low redshift evolution of dark energy (2004, background): “…which a field, typically a scalar field, provides the source of dark energy, e.g. quintessence (de la Macorra & Piccinelli 2000; GonzalezDiaz 2002; Urena-Lopez & Matos 2000; de Ritis & Marino 2001; Bludman & Roos 2002; Rubano & Scudellaro 2002; Sen & Seshadri 2003; Steinhardt 2003), k-essence…”
The Cosmological Constant and Dark Energy (2002, background): “109 For examples see Chimento and Jakubi (1996), Starobinsky (1998), Kruger and Norbury (2000), Di Pietro and Demaret (2001), Ureña-López and Matos (2000), González-Dı́az (2000), and Johri (2001).”