Inflationary energy scales, cosmic strings and textures

Details Inflationary energy scales, cosmic strings and textures Inflationary energy scales, cosmic strings and textures

Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990phlb..246..359l&link_type=abstract

Physics Letters B, Volume 246, Issue 3-4, p. 359-364.

Physics

22

Scientific paper

If there is an inflationary epoch, quantum fluctuations of the inflaton field give a contribution to the primeval spectrum of energy density perturbations, which can be calculated in terms of the inflaton potential. It is known that as a result observational constraints on the primeval spectrum of energy density perturbations provide an upper bound on the energy density during inflation, at the epoch when observable scales leave the horizon. Such a bound is here derived in a form requiring only weak and precisely formulated assumptions, and in addition tighter bounds are obtained on the energy density at the end of inflation and at reheating. With the bounds in mind, some aspects of spontaneous symmetry breaking are considered. Although it has more general applicability, the discussion focuses on the case of galaxy-forming cosmic strings or textures. It is shown that such objects probably cannot form after reheating, but that they can form at some earlier epoch if the scalar field involved has suitable interactions.

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