Schematic of confinement of matter to the brane, while gravity propagates in the bulk (from [51]).
The RS 2-brane model. (Figure taken from [58].)
Gravitational field of a small point particle on the brane in RS gauge. (Figure taken from [105].)
The evolution of the dimensionless shear parameter
on a
Bianchi I brane, for a 
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].)
The relation between the inflaton mass
(
) and the brane tension 
necessary to satisfy the COBE constraints. The
straight line is the approximation used in Equation ( 214
), which at high energies is in excellent agreement
with the exact solution, evaluated numerically in slow-roll. (Figure taken
from [222].)
Constraints from WMAP data on inflation models with quadratic and quartic potentials, where
is the ratio of tensor to scalar amplitudes
and 
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-
and 2-
contours are also shown. (Figure taken
from [203].)
Brane-world instanton. (Figure taken from [104].)
The evolution of the covariant variable
, defined in
Equation ( 298) (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 
, 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)]](article841x.gif)
, where 
is a small positive parameter (chosen as
in the plot). Labels on the curves indicate the
value of 
, so that the general
relativistic solution is the dashed
curve (
). (Figure taken
from [122].)
The evolution of
in the radiation era, with dark radiation present
in the background. (Figure taken
from [131].)
Graviton “volcano” potential around the
brane, showing the mass gap.
(Figure taken from [186].)
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.
and 
is a parameter giving the location of the regulator brane. (Figure
taken from [142].)
The CMB power spectrum with brane-world effects, encoded in the dark radiation fluctuation parameter
as a proportion of the large-scale curvature
perturbation for matter (denoted 
in the plot).
(Figure taken from [177].)
The CMB power spectrum with brane-world moduli effects from the field
in Equation ( 385). The curves are labelled with the initial value
of 
. (Figure taken from [268, 37].)