10 pp.
10 pp.
| 445 K 10 pp. | |
| View Document | ||
| Title | Inflationary Axion Cosmology | |
| Author(s) | Wilczek, Frank; Turner, Michael S. | |
| Publication Date | September 1990 | |
| Report Number | FERMILAB-Pub-90/198-A | |
| Unique Identifier | ACC0086 | |
| Other Numbers | OSTI ID: 6099352 | |
| Research Org | Fermi National Accelerator Laboratory; Enrico Fermi Institute, The University of Chicago; Institute for Advanced Study, School of Natural Sciences, Princeton, New Jersey | |
| Contract No | US Department of Energy (DOE) | |
| Subject | 640106 -- Astrophysics & Cosmology-- Cosmology ; 645103 -- High Energy Physics-- Particle Interactions & Properties-Experimental-- Strong Interactions & Baryon & Meson Properties; Axions-- Mass; Cosmology-- Axions; Inflationary Universe; Goldstone Bosons; Limiting Values; Phase Transformations; Quantum Chromodynamics; Scalar Fields; Symmetry Breaking | |
| Keywords | Bosons; Cosmological Models; Elementary Particles; Field Theories; Goldstone Bosons; Mathematical Models; Postulated Particles; Quantum Field Theory | |
| Related Web Pages | Frank Wilczek, Asymptotic Freedom, and Strong Interaction | |
| Abstract | If Peccei-Quinn (PQ) symmetry is broken after inflation, the initial axion angle is a random variable on cosmological scales; based on this fact, estimates of the relic-axion mass density give too large a value if the axion mass is less than about 10-6 eV. This bound can be evaded if the Universe underwent inflation after PQ symmetry breaking and if the observable Universe happens to be a region where the initial axion angle was atypically small, .1 . (ma/10-6eV)0.59. We show consideration of fluctuations induced during inflation severely constrains the latter alternative. | |
| 445 K 10 pp. | |
| View Document | ||
