1989
DOI: 10.1103/physrevd.39.405
|View full text |Cite
|
Sign up to set email alerts
|

Behavior of chaotic inflation in anisotropic cosmologies with nonminimal coupling

Help me understand this report

Search citation statements

Order By: Relevance

Paper Sections

Select...
2
1
1
1

Citation Types

1
84
0

Year Published

1993
1993
2018
2018

Publication Types

Select...
4
3

Relationship

0
7

Authors

Journals

citations
Cited by 70 publications
(85 citation statements)
references
References 12 publications
1
84
0
Order By: Relevance
“…Inflation in itself, without the use of singular equations or otherwise indeterminate evolutions, cannot wholly explain present isotropy or homogeneity, although it may reduce deviations by large factors [Sirousse-Zia, 1982, Wald, 1983, Moss and Sahni, 1986, Futamase et al, 1989. Although one can argue that anisotropy tends to prolong inflation, this does not remove the difficulty.…”
Section: Removal Of Anisotropy and Inhomogeneitymentioning
confidence: 99%
“…Inflation in itself, without the use of singular equations or otherwise indeterminate evolutions, cannot wholly explain present isotropy or homogeneity, although it may reduce deviations by large factors [Sirousse-Zia, 1982, Wald, 1983, Moss and Sahni, 1986, Futamase et al, 1989. Although one can argue that anisotropy tends to prolong inflation, this does not remove the difficulty.…”
Section: Removal Of Anisotropy and Inhomogeneitymentioning
confidence: 99%
“…Preliminary results [4,30] show that the convergence to the k = 0 FLRW universe can disappear by going from ξ = 0 to ξ = 0. Our perturbation analysis of Sec.…”
Section: Cosmic No-hair Theoremsmentioning
confidence: 99%
“…Even though the shift is small, it can have a tremendous effect on an inflationary scenario. The classical example of this effect is related to chaotic inflation [28]: the shift ξ = 0 → ξ renormalized = 10 −1 (a typical value predicted by renormalization [29]) is sufficient to ruin the chaotic inflationary scenario with potential V = λφ 4 [28,30]. Another reason to include a ξ = 0 term in the coupled Einstein-Klein-Gordon equations is that it is required by renormalization of the theory (this was the motivation for the introduction of NMC by Callan, Coleman and Jackiw [21]).…”
Section: Why ξ = 0 ?mentioning
confidence: 99%
See 1 more Smart Citation
“…Here, the authors obtained different constraints on the parameter coupling ξ ; also see Refs. [41][42][43][44]. As regards the relation between the tensor-to-scalar ratio and the scalar spectral index the consistency relation was studied in Refs.…”
Section: Introductionmentioning
confidence: 99%