CoChat
Sign Up
Cited by 142Cosmology and Gravitation TheoriesNoncommutative and Quantum Gravity TheoriesBlack Holes and Theoretical Physics

Non-Gaussianity from preheating

Open access
Enqvist, Kari, Jokinen, Asko, Mazumdar, Anupam, Multamäki, Tuomas, Väihkönen, Antti·2005·Physical Review Letters
DOI 10.1103/physrevlett.94.161301
Open this paper in CoChat — free accountOpen PDF

Abstract

We consider a two-field model for inflation where the second order metric perturbations can be amplified by a parametric resonance during preheating. We demonstrate that there can arise a considerable enhancement of non-Gaussianity sourced by the local terms generated through the coupled perturbations. We argue that the non-Gaussianity parameter could be as large as f(NL) approximately 50. Our results may provide a useful test of preheating in future cosmic microwave background experiments.

The claims and statistics of this paper haven’t been checked yet.

Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.

A few free checks a day · papers already verified open instantly · results are public

Integrity signals

Registry

Crossref · 10.1103/physrevlett.94.161301

Cites

1 of 1 references verified0 citation errors · 0 not checkable

Statistics

Claims the paper makes

The claims and statistics of this paper haven’t been checked yet.

Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.

A few free checks a day · papers already verified open instantly · results are public

Claims other papers make about this one

Each is checked against this paper’s own text: does it say what the citing paper says it does?

  • Non-adiabatic perturbations produced during multi-field inflation can generate detectable non-Gaussianity in the density field after inflation, in models such as the curvaton scenario or reheating.

    “Furthermore, non-adiabatic perturbations produced during multi-field inflation can certainly generate detectable non-Gaussianity in the density field after inflation, in models such as the curvaton scenario [10] (see also [11]) or reheating [12, 13, 14, 15].”

    From Non-Gaussianities in two-field inflation (2006) · cites this paper as [14]

Self-check

Percentages, sums and reported differences re-computed from the paper’s own numbers.

The self-check needs the paper’s full text.

Cites

Flagged first, then by citations

Research works printed but not linked: 48

  1. J. H. Traschen and R. H. Brandenberger, Phys. Rev. D 42, 2491 (1990).
  2. L. Kofman, A. D. Linde, and A. A. Starobinsky, Phys. Rev. Lett. 76, 1011 (1996);
  3. Y. Shtanov, J. H. Traschen, and R. H. Brandenberger, Phys. Rev. D 51, 5438 (1995);
  4. L. Kofman, A. D. Linde, and A. A. Starobinsky, Phys. Rev. D 56, 3258 (1997).
  5. D. Cormier, K. Heitmann, and A. Mazumdar, Phys. Rev. D 65, 083521 (2002).
  6. B. A. Bassett, D. I. Kaiser, and R. Maartens, Phys. Lett. B 455, 84 (1999);
  7. K. Jedamzik and G. Sigl, Phys. Rev. D 61, 023519 (2000);
  8. F. Finelli and R. H. Brandenberger, Phys. Rev. Lett. 82, 1362 (1999);
  9. F. Finelli and R. H. Branden- berger, Phys. Rev. D 62, 083502 (2000).
  10. A. R. Liddle, D. H. Lyth, K. A. Malik, and D. Wands, Phys. Rev. D 61, 103509 (2000).
  11. V. F. Mukhanov, H. A. Feldman, and R. H. Brandenberger, Phys. Rep. 215, 203 (1992).
  12. M. Parry and R. Easther, Phys. Rev. D 59, 061301 (1999);
  13. R. Easther and M. Parry, Phys. Rev. D 62, 103503 (2000);
  14. F. Finelli and S. Khlebnikov, Phys. Lett. B 504, 309 (2001);
  15. F. Finelli and S. Khlebnikov, Phys. Rev. D 65, 043505 (2002).
  16. J. McDonald, Phys. Rev. D 66, 043525 (2002);
  17. K. Enqvist, S. Kasuya, and A. Mazumdar, Phys. Rev. Lett. 89, 091301 (2002);
  18. K. Enqvist, S. Kasuya, and A. Mazumdar, Phys. Rev. D 66, 043505 (2002).
  19. C. L. Bennett et al., Astrophys. J. Suppl. Ser. 148, 1 (2003).
  20. J. Maldacena, J. High Energy Phys. 05, 013 (2003).
  21. J. Martin, A. Riazuelo, and M. Sakellariadou, Phys. Rev. D 61, 083518 (2000);
  22. A. Gangui, J. Martin, and M. Sakellariadou, Phys. Rev. D 66, 083502 (2002).
  23. E. Komatsu, astro-ph/0206039; · arXiv
  24. D. S. Salopek and J. R. Bond, Phys. Rev. D 42, 3936 (1990);
  25. D. S. Salopek and J. R. Bond, Phys. Rev. D 43, 1005 (1991);
  26. A. Gangui, F. Lucchin, S. Matarrese, and S. Mollerach, Astrophys. J. 430, 447 (1994);
  27. M. Bruni, S. Matarrese, S. Mollerach, and S. Sonego, Classical Quantum Gravity 14, 2585 (1997);
  28. A. D. Linde and V. Mukhanov, Phys. Rev. D 56, R535 (1997);
  29. S. Matarrese, S. Mollerach, and M. Bruni, Phys. Rev. D 58, 043504 (1998);
  30. N. Bartolo, S. Matarrese, and A. Riotto, Phys. Rev. D 65, 103505 (2002);
  31. G. Rigopoulos, Classical Quantum Gravity 21, 1737 (2004);
  32. N. Bartolo, S. Matarrese, and A. Riotto, J. Cosmol. Astropart. Phys. 0401, 003 (2004);
  33. M. Zaldarriaga, Phys. Rev. D 69, 043508 (2004);
  34. P. Creminelli, J. Cosmol. Astropart. Phys. 0310, 003 (2003);
  35. H. Noh and J. Hwang, Phys. Rev. D 69, 104011 (2004);
  36. K. A. Malik and D. Wands, Classical Quantum Gravity 21, L65 (2004);
  37. I. Rigopoulos, E. P. S. Shellard, and B. J. W. van Tent, astro-ph/0410486. · arXiv
  38. F. Bernardeau and J. P. Uzan, Phys. Rev. D 66, 103506 (2002);
  39. F. Bernardeau and J. P. Uzan, Phys. Rev. D 67, 121301 (2003);
  40. I. Yi and E. T. Vishniac, Astrophys. J. Suppl. Ser. 86, 333 (1993).
  41. K. Enqvist and A. Vaihkonen, J. Cosmol. Astropart. Phys. 0409, 006 (2004).
  42. N. Bartolo, E. Komatsu, S. Matarrese, and A. Riotto, Phys. Rep. 402, 103 (2004).
  43. N. Bartolo, S. Matarrese, and A. Riotto, J. High Energy Phys. 04, 006 (2004).
  44. K. Enqvist, S. Kasuya, and A. Mazumdar, Phys. Rev. Lett. 90, 091302 (2003);
  45. K. Enqvist, A. Jokinen, S. Kasuya, and A. Mazumdar, Phys. Rev. D 68, 103507 (2003);
  46. K. Enqvist, S. Kasuya, and A. Mazumdar, Phys. Rev. Lett. 93, 061301 (2004);
  47. K. Enqvist, A. Mazumdar, and A. Perez-Lorenzana, Phys. Rev. D 70, 103508 (2004).
  48. A. R. Liddle and A. Mazumdar, Phys. Rev. D 61, 123507 (2000).

Cited by

Sorted by citations

Authors
Enqvist, K., Jokinen, A., Mazumdar, A., Multamäki, T., & Väihkönen, A.
Affiliations
University of Helsinki (FI)
ORCID
Venue
Physical Review Letters
Publisher
American Physical Society (APS)
Published
2005-04-29
Volume
94
Issue
16
Pages
161301-161301
ISSN
  • 0031-9007 (ISSN-L)
  • 1079-7114
DOI
10.1103/physrevlett.94.161301
OpenAlex
W2075724928
Cited by
142
References
1
Citations by year
2025: 2 · 2024: 4 · 2023: 1 · 2021: 1 · 2020: 5 · 2019: 1 · 2018: 3 · 2017: 2 · 2016: 3 · 2015: 2 · 2014: 5 · 2013: 8 · 2012: 12
FWCI
8.73
Type
journal article
Language
en
Open access
Licence
link.aps.org/licenses/aps-default-license (vor)
Locations
  • Physical Review Letters (publishedVersion)
  • PubMed (publishedVersion)
  • Lancaster EPrints (Lancaster University) (acceptedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • CERN Document Server (European Organization for Nuclear Research) (submittedVersion)
  • arXiv (Cornell University)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Cosmology and Gravitation Theories
  • Physical Sciences › Physics and Astronomy › Statistical and Nonlinear Physics › Noncommutative and Quantum Gravity Theories
  • Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Black Holes and Theoretical Physics
Keywords
preheating, non-Gaussianity, two-field inflation, parametric resonance, metric perturbations, second-order perturbation theory, local non-Gaussianity, cosmic microwave background, primordial power spectrum

About these checks

Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.

Statistics and arithmetic are recomputed, not judged.

Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.

What counts as a claim ›How we measure confidence ›How we check this ›

Are you an author, or do you see a problem with this page? Request a review