Saving the invisible axion

Details Saving the invisible axion Saving the invisible axion

Sep 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983phlb..129...51s&link_type=abstract

Physics Letters B, Volume 129, Issue 1-2, p. 51-56.

Physics

104

Scientific paper

Recently it has been shown that the energy density contributed today by coherent oscillations of the invisible axion field corresponds to Ω ⋍ 0.1 (ƒ;a/1012 GeV)11/9 (ƒ;a is the scale of peccei-Quinn SSB), apparently ruling out ƒ;a >~ O(1013 GeV). We propose a simple way to avoid this bound: entropy production when the temperature of the universe is between about 1 GeV and 1 MeV. The entropy might be produced by a first-order phase transition, or the out-of-equilibrium decays of a relic particle species. For ƒ;a ⋍ 1015 GeV, the entropy of the universe must be increased by a factor of O(102-103) to have Ωa ⋍ O(1). If inflation also occurs at a temperature ⋍1015 GeV, then the de Sitter space produced fluctuations in the axion field lead to a Zel'dovich-like spectrum of (isothermal) perturbations in the axion energy density, with amplitude about 10-4. It has recently been argued that in an axion-dominated universe such a spectrum could lead to the formation of of the structure observed in the universe today.

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