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The Backreaction Conjecture to explain Dark Energy

Explore the Backreaction Conjecture in explaining Dark Energy within the Standard Model of Cosmology, addressing challenges and proposing alternative laws of gravitation.

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The Backreaction Conjecture to explain Dark Energy

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

  2. The Standard Model G= T t 2 a(t) δij ?

  3. The Standard Model works ! Baryons ~ 5% Dark Matter ~ 27% Dark Energy ~ 68 % Radiation ~ 0.01% Astier et al. 2006

  4. The Standard Model does not work ! Baryons ~ 5% fundamental scalar field / new particles ? Dark Matter ~ 27% other laws of gravitation ? effect of geometrical inhomogeneities? Dark Energy ~ 68 % Radiation ~ 0.01% backreaction conjecture

  5. Acceleration in the Standard Model localacceleration ⅓ a(t) =V (t) global acceleration apparentacceleration t 2 a(t) δij Λ

  6. Generalizing the Standard Model 1/3 aD= VR 4g = - dt2 + gij dXi dXj a(t) Einstein Spacetime t gij t

  7. Averaging Einstein’s Equations Spatial Average on a compact domain : Restmass conservation on the domain D

  8. Non - Commutativity

  9. Kinematical Backreaction • AccelerationLaw : • Expansion Law : • ConservationLaw : • Integrability :

  10. Effective Friedmann Equations • EffectiveScalarField :`Morphon´ Buchert, Larena, Alimi arXiv: gr-qc / 0606020

  11. G=  T m+  Pm+ P = m+  Pm+ P =

  12. Volume Partitioning

  13. Volume Partitioning D M

  14. Volume Partitioning E D M υ = D M

  15. Structure formation and Dark Energy Roukema, Ostrowski, Buchert arXiv: 1303.4444

  16. Acceleration in the Multiscale Model Q D

  17. Acceleration in the Multiscale Model Wiegand, Buchert arXiv: 1002.3912

  18. Integral Properties of Relativistic Models • Averageisnon-friedmannian : • genericscalingsolutions : n = p • relativisticperturbationtheory : n = p = -1 • Averageisfriedmannianfor : • Locallyisotropicmodels (homogeneous) • Special LTB modelswithhomogeneouscurvature

  19. Global Gravitational Instability Averaged Cosmologies Near FRW Cosmologies: Q small Unstable Sectors : Q < 0 and <R> > 0 Q > 0 and <R> < 0 Buchert, Larena, AlimiarXiv: gr-qc / 0606020 Roy, Buchert, Carloni, ObadiaarXiv: 1103.1146

  20. Phase Space for  = 0

  21. Unstable Sectors  = 0 DM DE

  22. Dark Energy Sector  = 0 Q > 0 and <R> < 0 2 1/aD 1 1/aD 0 1/aD

  23. Volume-dominance of Voids QD ≈ 0 <> ≈0 : <R>D - 2  ≈– 6 HD2

  24. Sloan Digital Sky Survey - slices • 150000 galaxies E uclide a n Todai, Tokyo

  25. Observational Strategies C Template Metrics log(1+z) Larena, Alimi, Buchert, Kunz, CorasanitiarXiv: 0808.1161 Euclid

  26. Conclusions • structureformationchangesthegeometry of • theaveragecosmology • Dark Energy and Dark Matter exist in terms of • “curvatureenergies“ • qualitative understanding of themechanism • iscompleted and itworks in the right direction • quantitative understanding in terms of • non-perturbativemodelsis in progress • reinterpretation of observations !

  27. Further Reading : arXiv: gr-qc/0001056 0707.2153 1103.2016 1112.5335

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