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Research output: Contribution to Journal/Magazine › Journal article › peer-review
Research output: Contribution to Journal/Magazine › Journal article › peer-review
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TY - JOUR
T1 - The inflating curvaton
AU - Dimopoulos, Konstantinos
AU - Kohri, Kazunori
AU - Lyth, David
AU - Matsuda, Tomohiro
PY - 2012/3/12
Y1 - 2012/3/12
N2 - The primordial curvature perturbation zeta may be generated by some curvaton field sigma, which is negligible during inflation and has more or less negligible interactions until it decays. In the current scenario, the curvaton starts to oscillate while its energy density rho_sigma is negligible. We explore the opposite scenario, in which rho_sigma drives a few e-folds of inflation before the oscillation begins. In this scenario for generating zeta it is exceptionally easy to solve the eta-problem; one just has to make the curvaton a string axion, with anomaly-mediated susy breaking which may soon be tested at the LHC. The observed spectral index n can be obtained with a potential V~phi^p for the first inflation; p = 1 or 2 is allowed by the current uncertainty in n but the improvement in accuracy promised by Planck may rule out p = 1. The predictions include (i) running n'= 0.0026 (0.0013) for p = 1 (2) that will probably be observed, (ii) non-gaussianity parameter fNL ~ −1 that may be observed, (iii) tensor fraction r is probably too small to ever observed.
AB - The primordial curvature perturbation zeta may be generated by some curvaton field sigma, which is negligible during inflation and has more or less negligible interactions until it decays. In the current scenario, the curvaton starts to oscillate while its energy density rho_sigma is negligible. We explore the opposite scenario, in which rho_sigma drives a few e-folds of inflation before the oscillation begins. In this scenario for generating zeta it is exceptionally easy to solve the eta-problem; one just has to make the curvaton a string axion, with anomaly-mediated susy breaking which may soon be tested at the LHC. The observed spectral index n can be obtained with a potential V~phi^p for the first inflation; p = 1 or 2 is allowed by the current uncertainty in n but the improvement in accuracy promised by Planck may rule out p = 1. The predictions include (i) running n'= 0.0026 (0.0013) for p = 1 (2) that will probably be observed, (ii) non-gaussianity parameter fNL ~ −1 that may be observed, (iii) tensor fraction r is probably too small to ever observed.
U2 - 10.1088/1475-7516/2012/03/022
DO - 10.1088/1475-7516/2012/03/022
M3 - Journal article
VL - 03
SP - 0
EP - 8
JO - Journal of Cosmology and Astroparticle Physics
JF - Journal of Cosmology and Astroparticle Physics
SN - 1475-7516
M1 - JCAP03(2012)022
ER -