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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Curvaton<br />
Scalar field σ (Mollerach 1990; Linde&Mukhanov 1997; Enqvist&Sloth 2002; Lyth&Wands 2002)<br />
V (φ, σ) = V (φ) + 1 2 m2 σ 2 + hσ ¯ψψ<br />
During inflation H > m: Scale-invariant fluctuations<br />
After inflation m > H: Behaves like matter<br />
P = 1 − r<br />
3 ρ tot, r = ρ χ<br />
ρ tot<br />
Decays perturbatively to ψ particles ⇒ ζ conserved<br />
ζ = N(χ + δχ) = r decay<br />
2<br />
δχ<br />
χ + r decay<br />
4<br />
( δχ<br />
χ<br />
) 2<br />
+ . . .<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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