Non-linear perturbations in relativistic cosmologyNon-linear perturbations in relativistic cosmology...
Transcript of Non-linear perturbations in relativistic cosmologyNon-linear perturbations in relativistic cosmology...
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Non-linear perturbations in relativistic cosmology
David Langlois(APC & IAP, Paris)
In collaboration with Filippo Vernizzi
• PRL ’05• PRD ’05• JCAP ’06• astro-ph/0610064
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Motivations• Linear theory of relativistic cosmological perturbations
extremely useful
• Non-linear aspects are needed in some cases:– non-gaussianities– Universe on very large scales (beyond the Hubble scales)– small scales
• Conservation laws– solve part of the equations of motion– useful to relate early universe
and ``late cosmology’’
Early Universegeometry
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Linear theory
• Perturbed metric (with only scalar perturbations)
• related to the intrinsic curvature of constant time spatial hypersurfaces
• Change of coordinates, e.g.
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Linear theory
• Curvature perturbation on uniform energy density hypersurfaces
• The time component of yields
For adiabatic perturbations, conserved on large scales
gauge-invariant
[Wands et al (2000)]
[Bardeen et al (1983)]
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Covariant formalism
• How to define unambiguously
• One needs a map
If is such that ,
then
• Idea: instead of , use its spatial gradient
[ Ellis & Bruni (1989) ]
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• Perfect fluid:
• Spatial projection:
• Expansion:
• Integrated expansion :
• Spatially projected gradients :
Local scale factor
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New approach
• Define
• Projection of along yields
• Spatial gradient
[ DL & Vernizzi, PRL ’05; PRD ’05 ]
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• One finally gets
• This is an exact equation, fully non-linear and val id at all scales !
• It “mimics” the linear equation
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Comparison with the coordinate based approach
• Choose a coordinate system
• Expand quantities:
• First order
Usual linear equation !
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• Second order perturbations
After some manipulations, one finds
in agreement with previous results [ Malik & Wands ’04]
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Gauge-invariance
• Second-order coordinate transformation
• ζa is gauge-invariant at 1st order but not 2nd order
• But, on large scales, and
is gauge-invariant on large scales!
Bruni et al. ‘97
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Cosmological scalar fields: single and multi-field inflation
• Multi-field inflation
– Generated fluctuations can be richer (adiabatic and isocurvature)– Adiabatic and isocurvature perturbations can be correlated
(D.L. ’99)– Decomposition into adiabatic & isocurvature modes
(Gordon et al. ‘01)
E.g. for two fields φ and χ, one can write
From Gordon et al. ‘01
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Cosmological scalar fields: covariant approach
• Several (minimally coupled) scalar fields
• Equation of motion
• Energy-momentum tensor
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Two scalar fields• Adiabatic and entropy directions
with
• Adiabatic and entropy covectors
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Equations of motion
• “Homogeneous-like” equations
• FLRW equations
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“Linear-like” equations
1. Evolution of the adiabatic covector
2. Evolution of the entropy covector
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Linearized equations
• First order spatial components of and
Second order equations for δσ and δs
• One usually replaces δσ by the gauge-invariant quantity
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Linearized equations
• Adiabatic equation
• Entropy equation
• On large scales,
[Gordon et al. ’01]
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Second order perturbations
• Entropy perturbation
• Adiabatic perturbation
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Large scale evolution
• Alternative adiabatic variable
• Using the 2nd order energy and moment constraints,
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Large scale evolution
• The entropy evolution on large scales is given by
• Evolution for ζ(2)
• Non-local term
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Conclusions
• New approach to study cosmological perturbations– Non linear– Purely geometric formulation (extension of the
covariant formalism)– ``Mimics’’ the linear theory equations – Get easily the second order results– Exact equations: no approximation
• Can be extended to scalar fields– Covariant and fully non-linear generalizations of the adiabatic
and entropy components– Evolution, on large scales, of the 2nd order adiabatic and entropy
components