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Scale-free primordial cosmology

Anna Ijjas*

Paul J. Steinhardt†

Abraham Loeb‡

  • Max-Planck-Institute for Gravitational Physics (Albert- Einstein-Institute), 14476 Potsdam, Germany and Rutgers University, New Brunswick, New Jersey 08901, USA

  • Department of Physics and Princeton Center for Theoretical Science, Princeton University, Princeton, New Jersey 08544, USA

  • Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts 02138, USA

  • *aijjas@princeton.edu
  • †steinh@princeton.edu
  • ‡aloeb@cfa.harvard.edu
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Phys. Rev. D 89, 023525 – Published 28 January, 2014

DOI: https://doi.org/10.1103/PhysRevD.89.023525

Abstract

The large-scale structure of the Universe suggests that the physics underlying its early evolution is scale-free. This was the historic motivation for the Harrison-Zel’dovich-Peebles spectrum and for inflation. Based on a hydrodynamical approach, we identify scale-free forms for the background equation of state for both inflationary and cyclic scenarios and use these forms to derive predictions for the spectral tilt and tensor-to-scalar ratio of primordial density perturbations. For the case of inflation, we find three classes of scale-free models with distinct predictions. Including all classes, we show that scale-free inflation predicts tensor-to-scalar ratio r>10−4. We show that the observationally favored class is theoretically disfavored because it suffers from an initial conditions problem and the hydrodynamical form of an unlikeliness problem similar to that identified recently for certain inflaton potentials. We contrast these results with those for scale-free cyclic models.

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Phys. Rev. D 89, 023525– Published 28 January, 2014
  • Received 8 October 2013

© 2014 American Physical Society

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