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Rapid Asymmetric Inflation and Early Cosmology in Theories with Sub-Millimeter Dimensions
High Energy Physics - Phenomenology · Submitted 2 Mar 1999
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We show that in such theories there exist attractive models of inflation that occur while the size of the new dimensions are still small.
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The abstract, sentence by sentence
It was recently pointed out that the fundamental Planck mass could be close to the TeV scale with the observed weakness of gravity at long distances being due the existence of new sub-millimeter spatial dimensions. In this picture the standard model fields are localized to a $(3+1)$-dimensional wall or ``3-brane''. We show that in such theories there exist attractive models of inflation that occur while the size of the new dimensions are still small. We show that it is easy to produce the required number of efoldings, and further that the density perturbations $\delta\rho/\rho$ as measured by COBE can be easily reproduced, both in overall magnitude and in their approximately scale-invariant spectrum. In the minimal approach, the inflaton field is just the moduli describing the size of the internal dimensions, the role of the inflationary potential being played by the stabilizing potential of the internal space. We show that under quite general conditions, the inflationary era is followed by an epoch of contraction of our world on the brane, while the internal dimensions slowly expand to their stabilization radius. We find a set of exact solutions which describe this behavior, generalizing the well-known Kasner solutions. During this phase, the production of bulk gravitons remains suppressed. The period of contraction is terminated by the blue-shifting of Hawking radiation left on our wall at the end of the inflationary de Sitter phase. The temperature to which this is reheated is consistent with the normalcy bounds. We give a precise definition of the radion moduli problem.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | It was recently pointed out that the fundamental Planck mass could be close to the TeV scale with the observed weakness of gravity at long distances being due the existence of new sub-millimeter spatial dimensions. | background 1.00 | 0.04 | 0.04 | hedged possibility 0.96 |
| s1 | In this picture the standard model fields are localized to a $(3+1)$-dimensional wall or ``3-brane''. | background 1.00 | 0.06 | 0.03 | asserted 0.99 |
| s2 | We show that in such theories there exist attractive models of inflation that occur while the size of the new dimensions are still small. | contribution 0.77 | 0.93 | 0.42 | asserted 0.98 |
| s3 | We show that it is easy to produce the required number of efoldings, and further that the density perturbations $\delta\rho/\rho$ as measured by COBE can be easily reproduced, both in overall magnitude and in their approximately scale-invariant spectrum. | result 0.98 | 0.92 | 0.17 | asserted 0.97 |
| s4 | In the minimal approach, the inflaton field is just the moduli describing the size of the internal dimensions, the role of the inflationary potential being played by the stabilizing potential of the internal space. | method 0.62 | 0.40 | 0.10 | asserted 0.90 |
| s5 | We show that under quite general conditions, the inflationary era is followed by an epoch of contraction of our world on the brane, while the internal dimensions slowly expand to their stabilization radius. | result 0.96 | 0.93 | 0.28 | asserted 1.00 |
| s6 | We find a set of exact solutions which describe this behavior, generalizing the well-known Kasner solutions. | contribution 0.53 | 0.96 | 0.08 | asserted 1.00 |
| s7 | During this phase, the production of bulk gravitons remains suppressed. | result 1.00 | 0.76 | 0.05 | asserted 0.99 |
| s8 | The period of contraction is terminated by the blue-shifting of Hawking radiation left on our wall at the end of the inflationary de Sitter phase. | result 0.95 | 0.69 | 0.08 | asserted 1.00 |
| s9 | The temperature to which this is reheated is consistent with the normalcy bounds. | result 0.93 | 0.73 | 0.06 | hedged possibility 0.75 |
| s10 | We give a precise definition of the radion moduli problem. | contribution 0.97 | 0.88 | 0.05 | asserted 0.96 |
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The paper
Original abstract
It was recently pointed out that the fundamental Planck mass could be close to the TeV scale with the observed weakness of gravity at long distances being due the existence of new sub-millimeter spatial dimensions. In this picture the standard model fields are localized to a $(3+1)$-dimensional wall or ``3-brane''. We show that in such theories there exist attractive models of inflation that occur while the size of the new dimensions are still small. We show that it is easy to produce the required number of efoldings, and further that the density perturbations $\delta\rho/\rho$ as measured by COBE can be easily reproduced, both in overall magnitude and in their approximately scale-invariant spectrum. In the minimal approach, the inflaton field is just the moduli describing the size of the internal dimensions, the role of the inflationary potential being played by the stabilizing potential of the internal space. We show that under quite general conditions, the inflationary era is followed by an epoch of contraction of our world on the brane, while the internal dimensions slowly expand to their stabilization radius. We find a set of exact solutions which describe this behavior, generalizing the well-known Kasner solutions. During this phase, the production of bulk gravitons remains suppressed. The period of contraction is terminated by the blue-shifting of Hawking radiation left on our wall at the end of the inflationary de Sitter phase. The temperature to which this is reheated is consistent with the normalcy bounds. We give a precise definition of the radion moduli problem.
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References
How the literature uses it
16 arXiv papers cite this in 27 sentences
Papers citing it · 20 sentences without a confident label
Builds on it 1 paper
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We will consider the framework of Ref. [ref] , outlined above, but depart from it by adding an interlude to the evolution of the cosmos before it ends up with stable extra dimensions.
Adagio for Thermal Relics · Models with Extra Dimensions · 0.88
Compares with it 2 papers
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(Unlike the Arkani-Hamed-Dimopoulous-Dvali (ADD) scenario [ref] , where $n > 2$ is generically allowed, in our case the chameleon constraints only allow $n=2$, as ([ref]) illustrates.)
Chameleonic inflation · Chameleon Region · 0.95
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We also note that our scenario differs from models in which the compact dimensions grow after inflation [ref] , or from scenarios in which the compact space inflates together with the three large spatial dimensions [ref] .
Curvature-Assisted Dynamical Compactification in a Pre-Inflationary Higher-Dimensional Universe · Curvature-assisted compactification before inflation · 0.99
Cites it as background 4 papers
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In typical scenarios for which Ref. [ref] aims to provide a cosmological framework, the radion eventually reaches the minimum of its potential where the extra dimensions attain their final stabilized size.
Adagio for Thermal Relics · Models with Extra Dimensions · 0.80
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The study of time-dependent cosmological backgrounds in string theory has a long history, including the study of the runaway epoch and generalisations of Kasner cosmologies (for example, see [ref] and for more recent work see [ref] ).
Kination, Meet Kasner: On The Asymptotic Cosmology of String Compactifications · Introduction · 1.00
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This approach offers new models describing, among others, inflation [ref] , the baryon asymmetry [ref] or the proton stability [ref] .
Solar axions in large extra dimensions · Introduction · 0.84
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