Cosmological Perturbations from Non-Equilibrium Quantum Fields
Cosmological Perturbations from Non-Equilibrium Quantum Fields
Cosmological Perturbations from Non-Equilibrium Quantum Fields
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Electrically Charged Curvaton<br />
Charged under electroweak U(1) (D’Onofrio,Lerner&AR 2012)<br />
Coleman-Weinberg potential<br />
V eff (σ) = m 2 |σ| 2 + 3g′4<br />
64π 2 |σ|4 ln<br />
( |σ|<br />
2<br />
µ 2 )<br />
Known coupling g ′ ≈ 0.357 (or integer multiple)<br />
During inflation:<br />
<strong>Perturbations</strong> mainly neutral (“Higgs mode”)<br />
Charge density screened by other charged particles<br />
After inflation:<br />
Perturbative decay (as usual)<br />
Interaction with thermal bath<br />
Parametric resonance with the gauge field<br />
Arttu Rajantie<br />
<strong>Cosmological</strong> <strong>Perturbations</strong> <strong>from</strong> <strong>Non</strong>-<strong>Equilibrium</strong> <strong>Quantum</strong> <strong>Fields</strong> – SEWM 2012
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