TY - JOUR

T1 - Quantum corrected mode function and power spectrum for a scalar field during inflation

AU - Onemli, V. K.

PY - 2014/4/30

Y1 - 2014/4/30

N2 - We compute the one- and two-loop corrected mode function of a massless minimally coupled scalar endowed with a quartic self-interaction in the locally de Sitter background of an inflating universe for a state which is released in Bunch-Davies vacuum at time t=0. We then employ it to correct the scalar's tree-order scale invariant power spectrum Δφ2. The corrections are secular, and have a scale-dependent part that can be expanded in even powers of k/(Ha), where k is the comoving wave number, H is the expansion rate and, a is the cosmic scale factor. At one-loop, the scale invariant shift in the power spectrum grows as (Ht)2 in leading order. The k-dependent shifts, however, are constants for each mode, in the late time limit. At two-loop order, on the other hand, the scale invariant shift grows as (Ht)4 whereas the k-dependent shifts grow as (Ht)2, in leading order. We finally calculate the scalar's spectral index nφ and the running of the spectral index αφ. They imply that the spectrum is slightly red-tilted; hence, the amplitudes of fluctuations grow slightly toward the larger scales.

AB - We compute the one- and two-loop corrected mode function of a massless minimally coupled scalar endowed with a quartic self-interaction in the locally de Sitter background of an inflating universe for a state which is released in Bunch-Davies vacuum at time t=0. We then employ it to correct the scalar's tree-order scale invariant power spectrum Δφ2. The corrections are secular, and have a scale-dependent part that can be expanded in even powers of k/(Ha), where k is the comoving wave number, H is the expansion rate and, a is the cosmic scale factor. At one-loop, the scale invariant shift in the power spectrum grows as (Ht)2 in leading order. The k-dependent shifts, however, are constants for each mode, in the late time limit. At two-loop order, on the other hand, the scale invariant shift grows as (Ht)4 whereas the k-dependent shifts grow as (Ht)2, in leading order. We finally calculate the scalar's spectral index nφ and the running of the spectral index αφ. They imply that the spectrum is slightly red-tilted; hence, the amplitudes of fluctuations grow slightly toward the larger scales.

UR - http://www.scopus.com/inward/record.url?scp=84899729409&partnerID=8YFLogxK

U2 - 10.1103/PhysRevD.89.083537

DO - 10.1103/PhysRevD.89.083537

M3 - Article

AN - SCOPUS:84899729409

SN - 1550-7998

VL - 89

JO - Physical Review D - Particles, Fields, Gravitation and Cosmology

JF - Physical Review D - Particles, Fields, Gravitation and Cosmology

IS - 8

M1 - 083537

ER -