Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005tsra.conf..338l&link_type=abstract
Proceedings of the 22nd Texas Symposium on Relativistic Astrophysics at Stanford, Stanford California, December 13-17, 2004. Ed
Astronomy and Astrophysics
Astrophysics
Scientific paper
Homogeneity and correlations in the observed CMB are indicative of some form of cosmological coherence in earlier times. Cosmological dark energy de-coherence is assumed to occur when the rate of expansion of the microscopically relevant cosmological scale parameter in the Friedmann-Lemaitre equations at early times is no longer supra-luminal. This choice of the scale parameter in the FL equations directly relates the scale of dark energy de-coherence to the De Sitter scale (associated with the positive cosmological constant) at late times. It is shown that the class of dynamical models so defined necessarily requires a spatially flat cosmology in order to be consistent with observed structure formation. Prior to de-coherence, the coherence which preserves the uniform density needed to make the FL dynamical equations meaningful must be maintained by supra-luminal (cosmological) correlations and not by the luminal or sub-luminal microscopic exchanges available after decoherence. The basic assumption is that the dark energy density which is fixed during de-coherence is to be identified with the cosmological constant. This approach makes no assumption about the constancy of dark energy density outside of the finite time interval when the expansion rate is not supra-luminal. It is shown for the entire class of models that the expected amplitude of fluctuations driven by the dark energy de-coherence process is of the order needed to evolve into the fluctuations observed in cosmic microwave background radiation and galactic clustering.
Lindesay James
Noyes Pierre H.
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