Wiggly whipped inflation
Abstract
Motivated by BICEP2 results on the CMB polarization Bmode which imply primordial gravitational waves are produced when the Universe has the expansion rate of about H ≈ 10{sup 14} GeV, and by deviations from a smooth powerlaw behavior for multipoles ℓ <50 in the CMB temperature anisotropy power spectrum found in the WMAP and Planck experiments, we have expanded our class of large field inflationary models that fit both the BICEP2 and Planck CMB observations consistently. These bestfitted large field models are found to have a transition from a faster roll to the slow roll V(φ)=m{sup 2} φ{sup 2}/2 inflation at a field value around 14.6 M{sub Pl} and thus a potential energy of V(φ) ∼ (10{sup 16} GeV){sup 4}. In general this transition with sharp features in the inflaton potential produces not only suppression of scalars relative to tensor modes at small k but also introduces wiggles in the primordial perturbation spectrum. These wiggles are shown to be useful to explain some localized features in the CMB angular power spectrum and can also have other observational consequences. Thus, primordial GW can be used now to make a tomography of inflation determining its fine structure. The resulting Wiggly Whipped Inflation scenario is described in details and the anticipatedmore »
 Authors:
 Asia Pacific Center for Theoretical Physics, Pohang, Gyeongbuk 790784 (Korea, Republic of)
 Paris Centre for Cosmological Physics, APC (CNRS), Université Paris Diderot, Université Sorbonne Paris Cité, Paris 75013 (France)
 Landau Institute for Theoretical Physics RAS, Moscow 119334 (Russian Federation)
 Publication Date:
 OSTI Identifier:
 22373379
 Resource Type:
 Journal Article
 Resource Relation:
 Journal Name: Journal of Cosmology and Astroparticle Physics; Journal Volume: 2014; Journal Issue: 08; Other Information: Country of input: International Atomic Energy Agency (IAEA)
 Country of Publication:
 United States
 Language:
 English
 Subject:
 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ANISOTROPY; COSMOLOGICAL INFLATION; FINE STRUCTURE; FREQUENCY ANALYSIS; GRAVITATIONAL WAVES; PERTURBATION THEORY; POLARIZATION; POTENTIAL ENERGY; POTENTIALS; SPECTRA; UNIVERSE
Citation Formats
Hazra, Dhiraj Kumar, Shafieloo, Arman, Smoot, George F., and Starobinsky, Alexei A., Email: dhiraj@apctp.org, Email: arman@apctp.org, Email: gfsmoot@lbl.gov, Email: alstar@landau.ac.ru. Wiggly whipped inflation. United States: N. p., 2014.
Web. doi:10.1088/14757516/2014/08/048.
Hazra, Dhiraj Kumar, Shafieloo, Arman, Smoot, George F., & Starobinsky, Alexei A., Email: dhiraj@apctp.org, Email: arman@apctp.org, Email: gfsmoot@lbl.gov, Email: alstar@landau.ac.ru. Wiggly whipped inflation. United States. doi:10.1088/14757516/2014/08/048.
Hazra, Dhiraj Kumar, Shafieloo, Arman, Smoot, George F., and Starobinsky, Alexei A., Email: dhiraj@apctp.org, Email: arman@apctp.org, Email: gfsmoot@lbl.gov, Email: alstar@landau.ac.ru. Fri .
"Wiggly whipped inflation". United States.
doi:10.1088/14757516/2014/08/048.
@article{osti_22373379,
title = {Wiggly whipped inflation},
author = {Hazra, Dhiraj Kumar and Shafieloo, Arman and Smoot, George F. and Starobinsky, Alexei A., Email: dhiraj@apctp.org, Email: arman@apctp.org, Email: gfsmoot@lbl.gov, Email: alstar@landau.ac.ru},
abstractNote = {Motivated by BICEP2 results on the CMB polarization Bmode which imply primordial gravitational waves are produced when the Universe has the expansion rate of about H ≈ 10{sup 14} GeV, and by deviations from a smooth powerlaw behavior for multipoles ℓ <50 in the CMB temperature anisotropy power spectrum found in the WMAP and Planck experiments, we have expanded our class of large field inflationary models that fit both the BICEP2 and Planck CMB observations consistently. These bestfitted large field models are found to have a transition from a faster roll to the slow roll V(φ)=m{sup 2} φ{sup 2}/2 inflation at a field value around 14.6 M{sub Pl} and thus a potential energy of V(φ) ∼ (10{sup 16} GeV){sup 4}. In general this transition with sharp features in the inflaton potential produces not only suppression of scalars relative to tensor modes at small k but also introduces wiggles in the primordial perturbation spectrum. These wiggles are shown to be useful to explain some localized features in the CMB angular power spectrum and can also have other observational consequences. Thus, primordial GW can be used now to make a tomography of inflation determining its fine structure. The resulting Wiggly Whipped Inflation scenario is described in details and the anticipated perturbation power spectra, CMB power spectra, nonGaussianity and other observational consequences are calculated and compared to existing and forthcoming observations.},
doi = {10.1088/14757516/2014/08/048},
journal = {Journal of Cosmology and Astroparticle Physics},
number = 08,
volume = 2014,
place = {United States},
year = {Fri Aug 01 00:00:00 EDT 2014},
month = {Fri Aug 01 00:00:00 EDT 2014}
}

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