Dark energy without dark energy

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• David L Wiltshire (Canterbury U.)
• Monday 26 May 2008, 13:00-14:00
• Potter Room, CMS, Pav.B, First Floor Common Room (B1.19).

If you have a question about this talk, please contact David Mulryne.

I present an unexpected explanation for dark energy [1], purely within general relativity with matter obeying the strong energy condition. Cosmic acceleration is explained quantitatively, as an apparent effect due to quasilocal gravitational energy differences – and hence clock rate variance – that arise in the decoupling of bound systems from the global expansion of the universe. Although the universe was initially very smooth, today it is very inhomogeneous on scales less than 200 Mpc, with clusters of galaxies strung in filaments and bubbles surrounding huge voids. Accounting for spatial curvature and gravitational energy gradients between galaxies and the volume average location in voids, leads to a recalibration of average cosmological parameters.

I present a model [1,2] of the universe based on this proposal, which passes three key independent cosmological tests [3]: supernova luminosity distances, the angular scale of the sound horizon in the cosmic microwave background (CMB) and the baryon acoustic oscillation scale in galaxy clustering statistics. It may simultaneously resolve particular anomalies, including primordial lithium abundances and CMB ellipticity. The expansion age is increased allowing more time for structure formation. Best-fit parameters and implications will be discussed. Unique predictions include a quantifiable variance in the Hubble flow below the scale of apparent homogeneity, consistent with the observed “Hubble bubble” feature, which sheds new light on the decades long debate about the value of the Hubble constant.

[1] D.L. Wiltshire, New J. Phys. 9 (2007) 377 [2] D.L. Wiltshire, Phys. Rev. Lett. 99 (2007) 251101 [3] B.M. Leith, S.C.C. Ng and D.L. Wiltshire, ApJ 672 (2008) L91

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