Fully Nonlinear and Exact Cosmological Perturbation...
Transcript of Fully Nonlinear and Exact Cosmological Perturbation...
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Fully Nonlinear and Exact Cosmological
Perturbation Theory
J. Hwang & H. Noh
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Newton’s theory: Non-relativistic (no c)
Action at a distance, violate causality
c=∞ limit of Einstein’s gravity: 0th
post-Newtonian limit
No horizon
Static nature
No strong pressure
No strong gravity
No gravitational waves
Incomplete and inconsistent
Einstein’s gravity: Relativistic
Strong gravity, dynamic
Simplest
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Perturbation method: Perturbation expansion
All perturbation variables are small
Weakly nonlinear
Strong gravity; fully relativistic
Valid in all scales
Fully nonlinear and Exact perturbations arXiv:1207.0264
Post-Newtonian method: Abandon geometric spirit of GR: recover the good old
absolute space and absolute time
Newtonian equations of motion with GR corrections
Expansion in strength of gravity
Fully nonlinear
No strong gravity; weakly relativistic
Valid far inside horizon
Case of the Fully nonlinear and Exact perturbations
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Fully
Relativistic
Weakly
Relativistic
Weakly
Nonlinear
?
Relativistic vs. Nonlinear Plane of Large-scale Structure
Newtonian
Gravity axis
Linear Perturbation
Background World
Model axis
Fully
Nonlinear
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Fully
Relativistic
Weakly
Relativistic
Post-Newtonian (PN)
Approximation
Per
turb
atio
n
Th
eory
(P
T)
Terra IncognitaNumerical Relativity
Weakly
Nonlinear
Newtonian
Gravity axis
Background World
Model axis
Perturbation vs. Post-Newtonian
Fully
Nonlinear
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Fully
Relativistic
Weakly
Relativistic
Terra IncognitaNumerical Relativity
Cosmological 1st order
Post-Newtonian (1PN)
Cosmological Nonlinear
Perturbation (2nd and 3rd order)
Perturbation vs. Post-Newtonian
Weakly
Nonlinear
Newtonian
Gravity axis
Linear Perturbation
Background World
Model axis
Fully
Nonlinear
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Fully
Relativistic
Weakly
Relativistic
Newtonian
Gravity axisFully
Nonlinear
Weakly
Nonlinear
Linear Perturbation
Fully NL and Exact Perturbation
Fully NL and Exact Pert. Eqs.
Terra IncognitaNumerical Relativity
Cosmological Nonlinear (NL)
Perturbation (2nd and 3rd order)
Cosmological 1st order
Post-Newtonian (1PN)
Background World
Model axis
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Newtonian Theory
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Mass conservation:
Momentum conservation:
Poisson’s equation:
Newtonian perturbation equations:
Newtonian (0PN) metric:
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Relativistic Theory
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Convention: (Bardeen 1988, York 1973)
Spatial gauge:
No anisotropic stress
No tensor-pert.
Complete spatial gauge fixing. Remaining variables are
spatially gauge-invariant to fully NL order!
Flat background
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Metric convention:
Energy-momentum tensor:
Inverse metric:
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To linear order:Perturbed Lapse Acceleration Curvature perturbation
Perturbed expansion Shear
Temporal gauge (slicing, hypersurface):
Nonlinear order
Complete gauge fixing, Remaining variables are gauge-
invariant to fully NL order!
Valid to NL order!
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Equations to linear order without taking temporal gauge condition: (Bardeen 1988)
Definition of kappa, Kii
ADM E-conservation, G00
ADM Mom-conservation, G0i
ADM propagation, trace, Gii
ADM propagation, tracefree, Gij- …
E-conservation, Tc0;c
Mom-conservation, Tci;c
Extended to fully Nonlinear order!
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E-conservation to NL order:
Covariant E-conservation
ADM E-conservationE-conservation
Covariant E-conservation:
As an example:
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Covariant E-conservation:
Comoving gauge + irrotational (vi = 0) + zero-pressure:
To 12th-order perturbation:
= 0, Background order
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Newtonian Limit
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c→∞ Limit in ZSG & UEG:
ZSG
ADM momentum-constraint
Tracefree ADM propagation
Covariant E-conservation
1
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Case with relativistic pressure:
Previous works were not successful in guessing the correct form.
(McCrea 1951; Harrison 1965; Coles & Lucchin 1995; Lima et al. 1997;
Harko 2011)
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Post-Newtonian Limit
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1PN convention: (Chandrasekhar 1965)
Identification:
Covariant E-conservation:
1PN equations! (JH, Noh & Puetzfeld 2008)
PT 1PN
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Fully NL and exact cosmological pert.:1. Formulation arXiv:1207.0264
2. Multi-component fluids
3. Minimally coupled scalar field
4. Newtonian limit arXiv:1210.0676
5. Relativistic pressure
6. 1PN equations
Future extentions:1. Anisotropic stress ⇒ Relativistic magneto-hydrodynamics
2. Background curvature
3. Light propagation (geodesic, Boltzmann)
4. 2 and higher-PN equations
5. Gauge-invariant combinations
Applications:1. NL perturbations
2. Fitting and Averaging
3. Backreaction
4. Relativistic cosmological numerical simulation
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