Aspects of Scalar Field Dynamics in Gauss-Bonnet Brane Worlds

TL;DR

This paper explores scalar field dynamics in Gauss-Bonnet brane worlds, analyzing inflationary models and perturbation ratios across different energy regimes, revealing how these models align with observational data.

Contribution

It investigates tachyon and scalar field inflation in Gauss-Bonnet brane worlds, highlighting the behavior of perturbation ratios and spectral indices across energy regimes and their observational implications.

Findings

Maximum scalar to tensor ratio near RS regime.

Suppressed ratio in high energy GB regime for positive p.

Models with polynomial potentials fit observational bounds across regimes.

Abstract

The Einstein-Gauss-Bonnet equations projected from the bulk to brane lead to a complicated Friedmann equation which simplifies to $H^2 \sim \rho^q$ in the asymptotic regimes. The Randall-Sundrum (RS) scenario corresponds to $q=2$ whereas $q=2/3$ $&$ $q=1$ give rise to high energy Gauss-Bonnet (GB) regime and the standard GR respectively. Amazingly, while evolving from RS regime to high energy GB limit, one passes through a GR like region which has important implications for brane world inflation. For tachyon GB inflation with potentials $V(\phi) \sim \phi^p$ investigated in this paper, the scalar to tensor ratio of perturbations $R$ is maximum around the RS region and is generally suppressed in the high energy regime for the positive values of $p$. The ratio is very low for $p>0$ at all energy scales relative to GB inflation with ordinary scalar field. The models based upon tachyon inflation with polynomial type of potentials with generic positive values of $p$ turn out to be in the $1 \sigma$ observational contour bound at all energy scales varying from GR to high energy GB limit. The spectral index $n_S$ improves for the lower values of $p$ and approaches its scale invariant limit for $p=-2$ in the high energy GB regime. The ratio $R$ also remains small for large negative values of $p$, however, difference arises for models close to scale invariance limit. In this case, the tensor to scale ratio is large in the GB regime whereas it is suppressed in the intermediate region between RS and GB. Within the frame work of patch cosmologies governed by $H^2 \sim \rho^q$, the behavior of ordinary scalar field near cosmological singularity and the nature of scaling solutions are distinguished for the values of $q < 1$ and $q > 1$.