cosmological nonlinear density and velocity power spectra€¦ · post-newtonian method: abandon...
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Cosmological Nonlinear Density and Velocity
Power Spectra
J. Hwang
UFES VitóriaNovember 11, 2015
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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
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
Excluding TT perturbation
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Fully
Relativistic
Weakly
Relativistic
Newtonian
Gravity axisFully
Nonlinear
Weakly
Nonlinear
Linear Perturbation
Relativistic vs. Nonlinear Pert.
Terra IncognitaNumerical Relativity
Cosmological Nonlinear (NL)
Perturbation (2nd and 3rd order)
Cosmological 1st order
Post-Newtonian (1PN)
Background World
Model axis`
Fully NL and Exact Pert. Eqs.
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Fully NL & Exact Pert. Theory
HJ & Noh, MNRAS 433 (2013) 3472
Noh, JCAP 07 (2014) 037
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The linear perturbations are so surprisingly simple that a
perturbation analysis accurate to second order may be
feasible using the methods of Hawking (1966). … One
could then judge the domain of validity of the linear
treatment and, more important, gain some insight into the
non-linear effects.
Sachs and Wolfe (1967)
Covariant (1+3) approach
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Convention: (Bardeen 1988)
Spatial gauge:
No anisotropic stress
Complete spatial gauge fixing.
Remaining variables are spatially gauge-invariant
to fully NL order! ∴ Lose no generality!
Decomposition, possible
to NL order (York 1973)
HJ & Noh, MNRAS 433 (2013) 3472; Noh, JCAP 07 (2014) 037
No TT-pert!
Spatial gauge condition
Temporal gauge still not taken yet!
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: Lorentz factor
Metric:
Energy-momentum tensor:
Four-vector:
Scalar- & vector-type decomposition:
Fluid three-velocity measured by Eulerian observer
Coordinate three-velocity of fluid
Internal energy
HJ & Noh, MNRAS 433 (2013) 3472; Noh, JCAP 07 (2014) 037
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Metric convention:
Inverse metric:
Using the ADM and the covariant formalisms the rest are simple algebra.We do not even need the connection!
HJ & Noh, MNRAS 433 (2013) 3472; Noh, JCAP 07 (2014) 037
Exact!
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Fully Nonlinear Perturbation Equationswithout taking temporal gauge condition:
Noh, JCAP 07 (2014) 037
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Tensor-type
to linear order
Noh, JCAP 07 (2014) 037
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with
ADM energy-constraint Trace of ADM propagation Covariant E-conservation
To Background order:
Noh, JCAP 07 (2014) 037
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To linear order without taking temporal gauge condition: (Bardeen 1988)
Definition of kappa, Kii
ADM energy-conservation, G00
ADM momentum-conservation, G0i
ADM propagation, trace, Gii
ADM propagation, tracefree, Gij - …
Energy-conservation, Tc0;c
Momentum-conservation, Tci;c
Extrinsic curvature
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Lapse function:
Intrinsic curvature:
Trace of extrinsic curvature:
Meanings of variables:
Perturbed curvature
Lapse
Acceleration vector Shear tensorExpansion scalar
Trace-free extrinsic curvature:
Rotation tensor
Perturbed expansion
Shear
HJ & Noh, MNRAS 433 (2013) 3472; Noh, JCAP 07 (2014) 037
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Temporal gauge (slicing, hypersurface):
Fully NL formulationNot available
Complete gauge fixing.
Remaining variables are gauge-invariant to fully
NL order!
Applicable to NL orders!
v = 0 from third order in
the presence of vector –type
perturbation
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Zero-pressure Irrotational Fluid
HJ & Noh, MNRAS 433 (2013) 3472
Noh, JCAP 07 (2014) 037
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Energy-conservation to NL order:
Covariant energy-conservation
ADM energy-conservationEnergy-conservation
Covariant energy-conservation:
Conservation equations:
= 0
HJ & Noh, MNRAS 433 (2013) 3472; Noh, JCAP 07 (2014) 037
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Covariant energy-conservation:
Comoving gauge + irrotational (vi = 0) + zero-pressure:
To 12th-order perturbation, say:
= 0, Background order
Exact!
Comoving gauge + irrotational Zero-pressure
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Zero-pressure fluid in the comoving gauge
ADM momentum constraint:
Covariant energy-conservation:
Trace of ADM propagation:
RHS = pure Einstein’s gravity corrections,
starting from the third order, all involving
Exact equations:
Definition of kappa + ADM momentum constraint:
Identify:
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Linear-order:
Second-order:
Third-order:Pure relativistic correction
appearing from third order.
All involving φ.
Relativistic/Newtonian correspondence
to second order.
This equation is valid to fully nonlinear
order in Newtonian theory.
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Power spectra:
JH, Jeong & Noh , arXiv:1509.07534
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Jeong, et al., ApJ 722, 1 (2011)
Unreasonable effectiveness of Newton’s gravity in cosmology!
Vishniac MN 1983
Jeong et al 2011
Pure Einstein
Leading Nonlinear Density Power-spectrum in the Comoving gauge:
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TensorVector
Tensor
Vector
General Relativistic Continuity and Euler equations to Third order in the Comoving gauge:
JH, Jeong & Noh , arXiv:1509.07534
Newtonian
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PES
PEV
PET
PE
PN13
PN22
P
Nonlinear Density Power-spectrum with vector and tensor contributions:
JH, Jeong & Noh , arXiv:1509.07534
13
1313
13
11P
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Nonlinear Velocity Power-spectrum with vector and tensor contributions:
PES
PEV
PET
PE
PN13
PN22
P
13
1313
13
11P
JH, Jeong & Noh , arXiv:1509.07534
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Newtonian LimitChandrasekhar, ApJ (1965): 0PN, MinkowskiJH, Noh & Puetzfeld, JCAP (2008): cosmologicalHere: as a limit of FNL&E PTJH & Noh, JCAP 04 (2013) 035
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Infinite speed-of-light Limit in ZSG & UEG:
ADM momentum-constraint:
Tracefree ADM propagation:
Covariant energy-conservation:1ZSG1
1
Subhorizon limit
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Trace of ADM propagation:
Covariant energy-conservation:
Covariant momentum-conservation:
Equations in Newtonian limit:
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With Relativistic Pressure
Infinite speed-of-light limit, except for pressureJH & Noh, JCAP 10 (2013) 054
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Case with Relativistic Pressure:
Previous works were not successful in guessing the correct forms.
(Whittaker 1935; McCrea 1951; Harrison 1965; Coles & Lucchin 1995;
Lima et al. 1997; … ; Harko 2011)
Trace of ADM propagation:
Covariant energy-conservation:
Covariant momentum-conservation:
No pressure!
JH & Noh, JCAP 04 (2013) 035
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Post-Newtonian Approximation
Chandrasekhar, ApJ (1965): 1PN, MinkowskiJH, Noh & Puetzfeld, JCAP (2008): cosmologicalHere: as a limit of FNL&E PTNoh & JH, JCAP 08 (2013) 040
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1PN convention: (Chandrasekhar 1965)
Identification:
Covariant E-conservation:
1PN equations! (JH, Noh & Puetzfeld , JCAP 2008)
PT 1PN
~Shear
JH, Noh & Puetzfeld, JCAP 03 (2008) 010
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ADM momentum-constraint:
Trace of ADM propagation:
Covariant energy-conservation:
Tracefree ADM propagation:
Covariant momentum-conservation:
Basic 1PN Equations:
Fourth-order in perturbation!
JH, Noh & Puetzfeld , JCAP 03 (2008) 010; Noh & JH, JCAP 08 (2013) 040
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Gauge conditions:
JH, Noh & Puetzfeld, JCAP 03 (2008) 010
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Propagation speed issue
Under the general gauge:
Propagation speed is gauge dependent!
JH, Noh & Puetzfeld, JCAP 03 (2008) 010
Trace of ADM propagation:
of the potential
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Resolution using Weyl tensor:
Eij, Hij equations:. .
JH, Noh & Puetzfeld, JCAP 03 (2008) 010
. .
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Fully NL and exact cosmological pert.:1. Formulation MN 433 (2013) 3472
2. Multi-component fluids , fields arXiv: 1511.01360
3. Minimally coupled scalar field JCAP 07 (2014) 037
4. Newtonian limit JCAP 04 (2013) 035
5. with relativistic pressure JCAP 10 (2013) 054
6. 1PN equations JCAP 08 (2013) 040
Future extentions:1. Anisotropic stress ⇒ Relativistic magneto-hydrodynamics
2. Light propagation (geodesic, Boltzmann)
3. 2 and higher order PN equations
4. Gauge-invariant combinations
5. TT perturbation should be handled perturbatively
Applications:1. Relativistic NL perturbations
2. Fitting and Averaging
3. Backreaction
4. Relativistic cosmological numerical simulation
}