Conserved cosmological perturbations
Open accessAbstract
A conserved cosmological perturbation is associated with each quantity whose local evolution is determined entirely by the local expansion of the Universe. It may be defined as the appropriately normalized perturbation of the quantity, defined using a slicing of spacetime such that the expansion between slices is spatially homogeneous. To first order, on superhorizon scales, the slicing with unperturbed intrinsic curvature has this property. A general construction is given for conserved quantities, yielding the curvature perturbation $\ensuremath{\zeta}$ as well as other more recently considered conserved perturbations. The construction may be extended to higher orders in perturbation theory and even into the non-perturbative regime.
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.
Integrity signals
Registry
Cites
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.
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?
The paper explicitly calculated in this model the non-Gaussianity due to the three-point function for the field perturbations at Hubble exit, using the result of Seery and Lidsey [8], and showed that it is small, as previously argued by Lyth and Zaballa [37].
“However, we have explicitly calculated in this model the non-Gaussianity due to the three-point function for the field perturbations at Hubble exit, using the result of Seery and Lidsey [8], and shown that it is small, as previously argued by Lyth and Zaballa [37].”
From Non-Gaussianities in two-field inflation (2006) · cites this paper as [37]
Split into 2 atoms — 0 confirmed, 1 partially supported, 0 disputed, 0 misattributed, 1 unverifiable. Expand the claim to see per-atom verdicts.
Experimental — accuracy not yet measuredThe first term on the right hand side of Eq. (26) is momentum dependent and comes from the three-point correlation functions of the fields, computed by quantizing the perturbations inside the Hubble radius during inflation.
“The first term on the right hand side of Eq. (26) is momentum dependent and comes from the three-point correlation functions of the fields, Eq. (21), computed by quantizing the perturbations inside the Hubble radius during inflation [35, 37].”
From Non-Gaussianities in two-field inflation (2006) · cites this paper as [37]
The Introduction describes vacuum fluctuations of light fields during inflation, and Section II discusses conserving second-order perturbations produced during inflation. Neither passage addresses the claimed momentum-dependent term, its origin in field three-point correlations, or their calculation by quantizing perturbations inside the Hubble radius; searches for those terms found no supporting passage in our copy. (LLM, conf=0.74)
Experimental — accuracy not yet measured
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
No references could be resolved yet.
Research works printed but not linked: 32
- [1][1] D. N. Spergel et al. , arXiv:astro-ph/0302209. - · arXiv
- [2][2] H. V. Peiris et al. , arXiv:astro-ph/0302225. - · arXiv
- [4][4] G. Veneziano, arXiv:hep-th/0002094. - · arXiv
- [5][5] R. Brustein, M. Gasperini, M. Giovannini, V. F. Mukhanov and G. Veneziano, Phys. Rev. D 51 , 6744 (1995) [arXiv:hep-th/9501066]. - · arXiv
- [6][6] J. E. Lidsey, D. Wands and E. J. Copeland, Phys. Rept. 337 , 343 (2000) [arXiv:hepth/9909061]. -
- [7][7] J. Khoury, B. A. Ovrut, P. J. Steinhardt and N. Turok, Phys. Rev. D 64 , 123522 (2001) [arXiv:hep-th/0103239]; D. H. Lyth, Phys. Lett. B 524 , 1 (2002) [arXiv:hepph/0106153]. - · arXiv
- [8][8] J. Khoury, B. A. Ovrut, P. J. Steinhardt and N. Turok, Phys. Rev. D 66 , 046005 (2002) [arXiv:hep-th/0109050]; D. H. Lyth, Phys. Lett. B 526 , 173 (2002) [arXiv:hepph/0110007]. - · arXiv
- [9][9] R. Kallosh, L. Kofman and A. D. Linde, Phys. Rev. D 64 , 123523 (2001) [arXiv:hepth/0104073]. -
- [10][10] H. Liu, G. Moore and N. Seiberg, arXiv:gr-qc/0301001. - · arXiv
- [13][13] J. Martin and D. J. Schwarz, Phys. Rev. D 57 , 3302 (1998) [arXiv:gr-qc/9704049]. - · arXiv
- [14][14] D. Wands, K. A. Malik, D. H. Lyth and A. R. Liddle, Phys. Rev. D 62 , 043527 (2000) [arXiv:astro-ph/0003278]. - · arXiv
- [16][16] D. H. Lyth and D. Wands, Phys. Lett. B 524 , 5 (2002) [arXiv:hep-ph/0110002]. - · arXiv
- [17][17] T. Moroi and T. Takahashi, Phys. Lett. B 522 , 215 (2001) [arXiv:hep-ph/0110096]. - · arXiv
- [19][19] A. D. Linde and V. Mukhanov, Phys. Rev. D 56 , 535 (1997) [arXiv:astro-ph/9610219]. - · arXiv
- [20][20] K. Enqvist and M. S. Sloth, Nucl. Phys. B 626 , 395 (2002) [arXiv:hep-ph/0109214]. - · arXiv
- [21][21] V. Bozza, M. Gasperini, M. Giovannini and G. Veneziano, Phys. Lett. B 543 , 14 (2002) [arXiv:hep-ph/0206131]. - · arXiv
- [22][22] E. J. Copeland, R. Easther and D. Wands, Phys. Rev. D 56 , 874 (1997) [arXiv:hepth/9701082]. -
- [23][23] D. H. Lyth, C. Ungarelli and D. Wands, Phys. Rev. D 67 , 023503 (2003) [arXiv:astroph/0208055]. -
- [24][24] K. A. Malik, D. Wands and C. Ungarelli, Phys. Rev. D 67 , 063516 (2003) [arXiv:astroph/0211602]. -
- [25][25] M. Sasaki and T. Tanaka, Prog. Theor. Phys. 99 , 763 (1998) [arXiv:gr-qc/9801017]. - · arXiv
- [26][26] J. Maldacena, JHEP 0305 , 013 (2003) [arXiv:astro-ph/0210603]. - · arXiv
- [27][27] V. Acquaviva, N. Bartolo, S. Matarrese and A. Riotto, arXiv:astro-ph/0209156. - · arXiv
- [28][28] R. Brandenberger and F. Finelli, JHEP 0111 , 056 (2001) [arXiv:hep-th/0109004]. - · arXiv
- [29][29] R. Trotta, A. Riazuelo and R. Durrer, Phys. Rev. Lett. 87 , 231301 (2001) [arXiv:astroph/0104017]. -
- [30][30] L. Amendola, C. Gordon, D. Wands and M. Sasaki, Phys. Rev. Lett. 88 , 211302 (2002) [arXiv:astro-ph/0107089]. - · arXiv
- [31][31] C. Gordon and A. Lewis, arXiv:astro-ph/0212248. - · arXiv
- [32][32] D. H. Lyth and D. Wands, arXiv:astro-ph/0306500. - · arXiv
- [33][33] A. R. Liddle and D. H. Lyth, 'Cosmological inflation and large-scale structure,' Cambridge, UK: Univ. Pr. (2000) 400 p . -
- [35][35] I. P. Heard and D. Wands, Class. Quant. Grav. 19 , 5435 (2002) [arXiv:gr-qc/0206085]. - · arXiv
- [36][36] S. Gratton, J. Khoury, P. J. Steinhardt and N. Turok, arXiv:astro-ph/0301395. - · arXiv
- [37][37] R. Durrer and F. Vernizzi, Phys. Rev. D 66 , 083503 (2002) [arXiv:hep-ph/0203275]; C. Cartier, R. Durrer and E. J. Copeland, Phys. Rev. D 67 , 103517 (2003) [arXiv:hepth/0301198]. - · arXiv
- [38][38] M. Sasaki and E. D. Stewart, Prog. Theor. Phys. 95 , 71 (1996) [arXiv:astro-ph/9507001]. - · arXiv
Cited by
Sorted by citations
Non-Gaussianities in two-field inflation
Vernizzi, F., & Wands, D. (2006) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2006/05/019 · Cited by 274 · see citing works
Self-citation
- Authors
- Lyth, D. H., & Wands, D.
- Affiliations
- Lancaster University (GB)
- University of Portsmouth (GB)
- ORCID
- Wands, David
- Venue
- Physical Review D
- Publisher
- American Physical Society (APS)
- Published
- 2003-11-25
- Volume
- 68
- Issue
- 10
- ISSN
- 0556-2821 (ISSN-L)
- 1089-4918
- OpenAlex
- W2016891104
- Cited by
- 161
- References
- 0
- Citations by year
- 2026: 11 · 2025: 11 · 2024: 6 · 2023: 4 · 2022: 6 · 2021: 6 · 2020: 3 · 2019: 3 · 2018: 4 · 2017: 2 · 2016: 2 · 2015: 6 · 2014: 4 · 2013: 5 · 2012: 1
- FWCI
- 8.29
- Type
- journal article
- Language
- en
- Open access
- green
- arxiv.org
- Locations
- Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- Lancaster EPrints (Lancaster University) (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 › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Keywords
- curvature perturbations, superhorizon scales, perturbation theory, intrinsic curvature
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
