The Backreaction Conjecture to explain Dark Energy

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The Backreaction Conjecture to explain Dark Energy Thomas Buchert, CRALyon MPIK May 26, 2014

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The Backreaction Conjecture to explain Dark Energy. Thomas Buchert , CRALyon. MPIK May 26, 2014. The Standard Model . G  =  T . t. 2. a ( t ) δij. ?. The Standard Model works !. Baryons ~ 5%. Dark Matter ~ 27%. Dark Energy ~ 68 %. Radiation ~ 0.01%. - PowerPoint PPT Presentation

Transcript of The Backreaction Conjecture to explain Dark Energy

Page 1: The  Backreaction  Conjecture to explain Dark Energy

The Backreaction Conjectureto explain Dark Energy

Thomas Buchert, CRALyon

MPIK May 26, 2014

Page 2: The  Backreaction  Conjecture to explain Dark Energy

The Standard Model

G = T

? a(t) δij 2 t

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The Standard Model works ! Baryons

~ 5%

Radiation ~ 0.01%

Dark Energy~ 68 %

Dark Matter

~ 27%

Astier et al. 2006

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The Standard Model does not work ! Baryons

~ 5%

Radiation ~ 0.01%

Dark Energy~ 68 %

Dark Matter ~

27%

fundamental scalar field / new particles ?

other laws of gravitation ?

effect of geometricalinhomogeneities ?

backreactionconjecture

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Acceleration in the Standard Model

Λa(t) δij 2 t

local acceleration

global acceleration

apparent accelerationa(t) =V (t) ⅓

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Generalizing the Standard Model

t

1/3aD= VR

Einstein Spacetime

4g = - dt2 + gij dXi dXj

gijt

a(t)

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Averaging Einstein’s Equations

Spatial Average on a compact domain :

Restmass conservation on the domain D

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Non - Commutativity

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Acceleration Law :

Expansion Law :

Conservation Law :

Integrability :

Kinematical Backreaction

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Effective Friedmann Equations

Effective Scalar Field :`Morphon´

Buchert, Larena, Alimi arXiv: gr-qc / 0606020

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G = T

m +

Pm + P

m +

Pm + P

=

=

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Volume Partitioning

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Volume Partitioning

D

M

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Volume Partitioning

D

M

D EM= υ

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Structure formation and Dark Energy

Roukema, Ostrowski, Buchert arXiv: 1303.4444

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Acceleration in the Multiscale Model

Q D

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Acceleration in the Multiscale Model

Wiegand, Buchert arXiv: 1002.3912

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Average is friedmannian for :

Locally isotropic models (homogeneous) Special LTB models with homogeneous curvature

Integral Properties of Relativistic Models

Average is non-friedmannian :

generic scaling solutions : n = p relativistic perturbation theory : n = p = -1

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Unstable Sectors :

Q < 0 and <R> > 0

Q > 0 and <R> < 0

Averaged Cosmologies

Near FRW Cosmologies: Q small

Global Gravitational Instability

Roy, Buchert, Carloni, Obadia arXiv: 1103.1146

Buchert, Larena, Alimi arXiv: gr-qc / 0606020

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Phase Space for = 0

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Unstable Sectors = 0

DE

DM

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Dark Energy Sector = 0

1/aD

Q > 0 and <R> < 0

1/aD

0

21

1/aD

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<R>D - 2 ≈ – 6 HD2

QD ≈ 0 <> ≈ 0 :

Volume-dominance of Voids

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Sloan Digital Sky Survey - slices

Todai, Tokyo 150000 galaxies

E u c l i d e a n

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Observational Strategies

C

log(1+z)

Template Metrics

EuclidLarena, Alimi, Buchert, Kunz, Corasaniti arXiv: 0808.1161

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structure formation changes the geometry of the average cosmology

Dark Energy and Dark Matter exist in terms of “curvature energies“ qualitative understanding of the mechanism is completed and it works in the right direction

quantitative understanding in terms of non-perturbative models is in progress reinterpretation of observations !

Conclusions

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Further Reading :

arXiv:gr-qc/0001056

0707.21531103.20161112.5335