Power-Law Inflation from the Rolling Tachyon

By A. Feinstein. 2002

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Modeling the potential by an inverse square law in terms of the tachyon field $[V(T)=\ensuremath{\beta}{T}^{\ensuremath{-}2}]$ we find an exact solution for a spatially flat isotropic universe. We show that for $\ensuremath{\beta}g2\sqrt{3}/3$ the model undergoes power-law inflation. A way to construct other exact solutions is specified and exemplified.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/fb0fc10010f4c52c1a0deba336763cd93d1032d6

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Citations in the corpus

Cosmological parameters from supernova observations: A critical comparison of three data sets (2003, background): “…Wang, & Steinhardt 1999) and the other corresponding to the tachyonic scalar fields (Padmanabhan 2002; Padmanabhan & Choudhury 2002; Frolov, Kofman, & Starobinsky 2002; Shiu & Wasserman 2002; Gibbons 2002; Fairbairn & Tytgat 2002; Mukohyama 2002; Feinstein 2002; Bagla, Jassal, & Padmanabhan 2003).”
Tachyons, scalar fields, and cosmology (2003, methodology): “The scalar field model with the potential (36) was studied in [23] while the corresponding tachyon model with the potential (38) was discussed in [10, 11].”
Scalar speed limits and cosmology: Acceleration from D-cceleration (2003, background): “Of particular relevance for the present work is the observation [9] that the power-law inflationary phase of Case B can be obtained by the choice F (T ) ∼ 1/T 2 in the Lagrangian (5.”
Problems with Tachyon Inflation (2002, background): “In papers [24, 25] inflation was considered for phenomenological potentials V (T ) hat have not been derived in the string tachyon theory.”