Constraints on Parameters of Models With Extra Dimension From Primordial Nucleosynthesis

Iofa, Mikhail Z.

doi:10.1142/s0217732309031557

Cited by 2 publications

(5 citation statements)

References 23 publications

(52 reference statements)

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“…where we used that µM 2 pl /M 3 ≃ 1 [18,19]. Taking µ ∼ 10 −12 GeV , we find that the approximation of late cosmology is valid up to the temperatures of order 5 • 10 2 GeV .…”

Section: Period Of Late Cosmologymentioning

confidence: 82%

“…, where H0 is the present-time Hubble parameter [18,19]. For µ ∼ 10 −12 GeV correction is ∼ 10 −60 .…”

Section: Jcap06(2011)025mentioning

confidence: 99%

“…where the integrals I 04 and I 44 were defined in the previous section. We use also the 5D energy conservation equation (18) which is written aṡ…”

Section: Graviton Emission In the Period Of Late Cosmologymentioning

confidence: 99%

“…Substituting in this equation T (4)0 0 from (117) and expressing ρ via (18), we obtain (cf. [9,12]) ρD + 4Hρ D + 2κ 2 µ Ť04 (µ + ρ) + H Ť44 = 0.…”

Section: A 3d Brane In 5d Bulkmentioning

confidence: 99%

“…Assuming that the terms with the bulk energy-momentum 3 We assume invariance y ↔ −y. 4 From the 5D Einstein equations and the fit of the data on abundance of 4 He produced in nucleosynthesis it follows that σ 2 = µ 2 (1 + O(H 2 0 /µ 2 )), where H 0 is the present-time Hubble parameter [18,19]. For µ ∼ 10 −12 GeV correction is ∼ 10 −60 .…”

Section: Introductionmentioning

confidence: 99%

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Graviton emission from the brane in the bulk in a model with extra dimension

Iofa

2011

J. Cosmol. Astropart. Phys.

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In a model of 3-brane embedded in 5D space-time we calculate the graviton emission from the brane to the bulk. Matter is confined to the brane, gravitons produced in reactions of matter on the brane escape to the bulk. The Einstein equations which are modified by the terms due to graviton production are solved perturbatively, the leading order being that without the graviton production. In the period of late cosmology, in which in the generalized Friedmann equation the term linear in the energy density of matter in dominant, we calculate the spectrum of gravitons (of the tower of Kaluza-Klein states) and the collision integral in the Boltzmann equation. We find the energy-momentum tensor of the emitted gravitons in the bulk, and using it show that corrections due to graviton production to the leading-order terms in the Einstein equations are small, and the perturbative approach is justified. We calculate the difference of abundances of 4 He produced in primordial nucleosynthesis in the models with and without the graviton production, and find that the difference is a very small number, much smaller than that estimated previously.

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“…where we used that µM 2 pl /M 3 ≃ 1 [18,19]. Taking µ ∼ 10 −12 GeV , we find that the approximation of late cosmology is valid up to the temperatures of order 5 • 10 2 GeV .…”

Section: Period Of Late Cosmologymentioning

confidence: 82%

“…, where H0 is the present-time Hubble parameter [18,19]. For µ ∼ 10 −12 GeV correction is ∼ 10 −60 .…”

Section: Jcap06(2011)025mentioning

confidence: 99%

“…where the integrals I 04 and I 44 were defined in the previous section. We use also the 5D energy conservation equation (18) which is written aṡ…”

Section: Graviton Emission In the Period Of Late Cosmologymentioning

confidence: 99%

“…Substituting in this equation T (4)0 0 from (117) and expressing ρ via (18), we obtain (cf. [9,12]) ρD + 4Hρ D + 2κ 2 µ Ť04 (µ + ρ) + H Ť44 = 0.…”

Section: A 3d Brane In 5d Bulkmentioning

confidence: 99%