List of Figures

View Image Figure 1:
Schematic of confinement of matter to the brane, while gravity propagates in the bulk (from [51]).
View Image Figure 2:
The RS 2-brane model. (Figure taken from [58].)
View Image Figure 3:
Gravitational field of a small point particle on the brane in RS gauge. (Figure taken from [105].)
View Image Figure 4:
The evolution of the dimensionless shear parameter _O_shear = s2/6H2 on a Bianchi I brane, for a V = 12m2f2 model. The early and late-time expansion of the universe is isotropic, but the shear dominates during an intermediate anisotropic stage. (Figure taken from [221].)
View Image Figure 5:
The relation between the inflaton mass m/M 4 (M =_ M 4 p) and the brane tension 4 1/4 (c/M 4) necessary to satisfy the COBE constraints. The straight line is the approximation used in Equation ( 214View Equation), which at high energies is in excellent agreement with the exact solution, evaluated numerically in slow-roll. (Figure taken from [222].)
View Image Figure 6:
Constraints from WMAP data on inflation models with quadratic and quartic potentials, where R is the ratio of tensor to scalar amplitudes and n is the scalar spectral index. The high energy (H.E.) and low energy (L.E.) limits are shown, with intermediate energies in between, and the 1-s and 2-s contours are also shown. (Figure taken from [203].)
View Image Figure 7:
Brane-world instanton. (Figure taken from [104].)
View Image Figure 8:
The evolution of the covariant variable P, defined in Equation ( 298View Equation) (and not to be confused with the Bardeen potential), along a fundamental world-line. This is a mode that is well beyond the Hubble horizon at N = 0, about 50 e-folds before inflation ends, and remains super-Hubble through the radiation era. A smooth transition from inflation to radiation is modelled by w = 13[(2 - 32e)tanh(N - 50) - (1 - 32e)], where e is a small positive parameter (chosen as e = 0.1 in the plot). Labels on the curves indicate the value of r0/c, so that the general relativistic solution is the dashed curve (r /c = 0 0). (Figure taken from [122].)
View Image Figure 9:
The evolution of P in the radiation era, with dark radiation present in the background. (Figure taken from [131].)
View Image Figure 10:
Graviton “volcano” potential around the dS4 brane, showing the mass gap. (Figure taken from [186].)
View Image Figure 11:
Damping of brane-world gravity waves on horizon re-entry due to massive mode generation. The solid curve is the numerical solution, the short-dashed curve the low-energy approximation, and the long-dashed curve the standard general relativity solution. eE = r0/c and g is a parameter giving the location of the regulator brane. (Figure taken from [142].)
View Image Figure 12:
The CMB power spectrum with brane-world effects, encoded in the dark radiation fluctuation parameter dC* as a proportion of the large-scale curvature perturbation for matter (denoted z* in the plot). (Figure taken from [177].)
View Image Figure 13:
The CMB power spectrum with brane-world moduli effects from the field x in Equation ( 385View Equation). The curves are labelled with the initial value of x. (Figure taken from [268, 37].)