Inflationary axion cosmology.
Inflationary axion cosmology.
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暴胀轴子宇宙学。
DOI：
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发表时间：
1991
影响因子：
8.6
通讯作者：
F. Wilczek
中科院分区：
文献类型：
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作者：
M. Turner;M. Turner;F. Wilczek
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{sup {minus}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, {theta}{sub 1}{approx lt}({ital m}{sub {ital a}}/10{sup {minus}6} eV{sup 0.59}.) We show consideration of fluctuations induced during inflation severely constrains the latter alternative.
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{sup {minus}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, {theta}{sub 1}{approx lt}({ital m}{sub {ital a}}/10{sup {minus}6} eV{sup 0.59}.) We show consideration of fluctuations induced during inflation severely constrains the latter alternative.