Cosmological perturbation theory

In

, must be used. When deciding whether to use general relativity for perturbation theory, note that Newtonian physics is only applicable in some cases such as for scales smaller than the Hubble horizon, where spacetime is sufficiently flat, and for which speeds are non-relativistic.

Because of the

, the correct formulation of cosmological perturbation theory is subtle. In particular, when describing an inhomogeneous spacetime, there is often not a preferred coordinate choice. There are currently two distinct approaches to perturbation theory in classical general relativity:

• gauge-invariant perturbation theory based on foliating a space-time with hyper-surfaces, and
• 1+3 covariant gauge-invariant perturbation theory based on threading a space-time with frames.

Newtonian perturbation theory

In this section, we will focus on the effect of matter on structure formation in the hydrodynamical fluid regime. This regime is useful because dark matter has dominated structure growth for most of the universe's history. In this regime, we are on sub-Hubble scales ${\displaystyle <H^{-1}~,}$ (where ${\displaystyle H}$ is the

) so we can take spacetime to be flat, and ignore general relativistic corrections. But these scales are above a cut-off, such that perturbations in pressure and density are sufficiently linear ${\displaystyle \delta P~,~\delta \rho \ll 1~.}$ Next we assume low pressure ${\displaystyle P\ll \rho ~,}$ so that we can ignore radiative effects and low speeds ${\displaystyle u\ll c~,}$ so we are in the non-relativistic regime.

The first governing equation follows from matter conservation – the continuity equation^[6]

${\displaystyle {\frac {\partial \rho }{\partial t}}+3H\rho +{\frac {1}{a}}\cdot \nabla \left(\rho {\vec {v}}\right)=0~,}$

where ${\displaystyle a}$ is the scale factor and ${\displaystyle {\vec {v}}}$ is the peculiar velocity. Although we don't explicitly write it, all variables are evaluated at time ${\displaystyle t}$ and the divergence ${\displaystyle \nabla }$ is in comoving coordinates. Second, momentum conservation gives us the Euler equation

${\displaystyle \rho {\frac {{\text{d}}{\vec {u}}}{{\text{d}}t}}=\rho \left({\frac {\partial }{\partial t}}+{\frac {1}{a}}{\vec {v}}\cdot \nabla \right){\vec {u}}=-{\frac {1}{a}}\nabla P-{\frac {1}{a}}\rho \nabla \Phi ~,}$

where ${\displaystyle \Phi }$ is the gravitational potential. Lastly, we know that for Newtonian gravity, the potential obeys the Poisson equation

${\displaystyle {\frac {1}{a^{2}}}\nabla ^{2}\Phi =4\pi G\rho ~.}$

So far, our equations are fully nonlinear, and can be hard to interpret intuitively. It's therefore useful to consider a perturbative expansion and examine each order separately. We use the following decomposition

${\displaystyle \rho ={\bar {\rho }}(1+\delta )~,~{\vec {u}}=Ha{\vec {x}}+{\vec {v}}~,~P={\bar {P}}+\delta P~,~\Phi ={\bar {\Phi }}+\delta \Phi ~}$

where ${\displaystyle {\vec {x}}}$ is a comoving coordinate.

At linear order, the continuity equation becomes

${\displaystyle {\dot {\delta }}=-{\frac {1}{a}}\theta ~,}$

where ${\displaystyle \theta \equiv \nabla \cdot {\vec {v}}}$ is the velocity divergence. And the linear Euler equation is

${\displaystyle {\bar {\rho }}\left({\dot {\vec {v}}}+H{\vec {v}}\right)=-{\frac {1}{a}}\nabla \delta P-{\frac {1}{a}}{\bar {\rho }}\nabla \delta \Phi ~.}$

By combining the linear continuity, Euler, and Poisson equations, we arrive at a simple master equation governing evolution

${\displaystyle \left({\frac {\partial ^{2}}{\partial ^{2}t}}+2H{\frac {\partial }{\partial t}}-c_{s}^{2}{\frac {1}{a}}\nabla ^{2}-4\pi G{\bar {\rho }}\right)\delta =0~,}$

where we defined a sound speed ${\displaystyle c_{s}^{2}\equiv \delta P/{\bar {\rho }}\delta ~}$ to give us a closure relation. This master equation admits wave solutions in ${\displaystyle \delta ({\vec {x}},t)}$ which tell us how matter fluctuations grow over time due to a combination of competing effects – the fluctuation's self-gravity, pressure forces, the universe's expansion, and the background gravitational field.

Gauge-invariant perturbation theory

The gauge-invariant perturbation theory is based on developments by Bardeen (1980),

like analogue and usually has as it starting point the FRW background around which perturbations are developed. The approach is non-local and coordinate dependent but gauge invariant as the resulting linear framework is built from a specified family of background hyper-surfaces which are linked by gauge preserving mappings to foliate the space-time. Although intuitive this approach does not deal well with the nonlinearities natural to general relativity.

1+3 covariant gauge-invariant perturbation theory

In

Gauge freedom and frame fixing

In relativistic cosmology there is a freedom associated with the choice of threading frame; this frame choice is distinct from the choice associated with coordinates. Picking this frame is equivalent to fixing the choice of timelike world lines mapped into each other. This reduces the

gauge freedom

; it does not fix the gauge but the theory remains gauge invariant under the remaining gauge freedoms. In order to fix the gauge a specification of correspondences between the time surfaces in the real universe (perturbed) and the background universe are required along with the correspondences between points on the initial spacelike surfaces in the background and in the real universe. This is the link between the gauge-invariant perturbation theory and the gauge-invariant covariant perturbation theory. Gauge invariance is only guaranteed if the choice of frame coincides exactly with that of the background; usually this is trivial to ensure because physical frames have this property.

Newtonian-like equations

Newtonian-like equations emerge from perturbative general relativity with the choice of the Newtonian gauge; the Newtonian gauge provides the direct link between the variables typically used in the gauge-invariant perturbation theory and those arising from the more general gauge-invariant covariant perturbation theory.

See also

• Primordial fluctuations
• Cosmic microwave background spectral distortions

References

Bibliography

See physical cosmology textbooks.

External links

• Ellis, George F. R.; van Elst, Henk (1999). "Cosmological models". In Marc Lachièze-Rey (ed.). Theoretical and Observational Cosmology: Proceedings of the NATO Advanced Study Institute on Theoretical and Observational Cosmology. Cargèse Lectures 1998. NATO Science Series: Series C. Vol. 541.
  Bibcode:1999ASIC..541....1E
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