Tachyons, scalar fields, and cosmology

By V. Gorini, A. Kamenshchik, U. Moschella, V. Pasquier. 2003

242 citations recorded by the source corpus.

We study the role that tachyon fields may play in cosmology as compared to the well-established use of minimally coupled scalar fields. We first elaborate on a kind of correspondence existing between tachyons and minimally coupled scalar fields; corresponding theories give rise to the same cosmological evolution for a particular choice of the initial conditions but not for any other. This leads us to study a specific one-parameter family of tachyonic models based on a perfect fluid mixed with a positive cosmological constant. For positive values of the parameter, one needs to modify Sen's action and use the $\ensuremath{\sigma}$ process of resolution of singularities. The physics described by this model is dramatically different and much richer than that of the corresponding scalar field. For particular choices of the initial conditions, the universe, which does mimic for a long time a de Sitter\char21{}like expansion, ends up in a finite time in a special type of singularity that we call a big brake. This singularity is characterized by an infinite deceleration.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c705bca61da0bbc915928745915ff96a26f92e73

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Citations in the corpus

Dynamical systems applied to cosmology: Dark energy and modified gravity (2017, background): “Applications of tachyonic scalar fields to late time cosmology were considered soon after they arose from high-energy physics (Padmanabhan, 2002; Gibbons, 2002, 2003; Bagla et al., 2003; Gorini et al., 2004).”
WMAP constraints on low redshift evolution of dark energy (2004, background): “…2002; Shiu & Wasserman 2002; Bagla, Jassal & Padmanabhan 2003; Gibbons 2003a; Jassal 2004; Kim, Kim & 2003; Sen 2003; Aguirregabiria & Lazkoz 2004; Gorini et al. 2004), phantom fields (Caldwell 2002; Carroll et al. 2003; Dabrowski et al. 2003; Frampton 2003; Gibbons 2003b; Gonzalez-Diaz 2003b;…”
The Chaplygin gas as a model for dark energy (2004, unknown): “ar X iv :g rqc /0 40 30 62”