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Fibre Inflation High-Fibre models from regular potentials String Pheno Workshop: CERN 2008 C.P. Burgess with M. Cicoli and F.Quevedo
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String Phenomenology Workshop CERN 2008 Outline String inflation Why build models only a mother could love? Gravity waves and stringy signals? Fibre Inflation and the LVS Inflating with moduli Inflationary Observables Correlations between r and ns; gravity waves;…
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String Phenomenology Workshop CERN 2008 String Inflation What might one hope to learn? about strings about inflation
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String Phenomenology Workshop CERN 2008 String Inflation What might one hope to learn? about strings about inflation String Theory: a theory in search of observational tests Inflation: successful phenomenology seeking an underlying theory
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String Phenomenology Workshop CERN 2008 String Inflation What might one hope to learn? about strings about inflation … Rocky Kolb
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String Phenomenology Workshop CERN 2008 String Inflation What might one hope to learn? about strings about inflation Difficult to identify where we live within the string landscape. Seek ‘modules’ encoding low-energy features: standard model; dark energy; inflation; …
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String Phenomenology Workshop CERN 2008 String Inflation What might one hope to learn? about strings about inflation Inflation provides a good description of primordial fluctuations as seen in the CMB: a rare observational window on physics at high energies? Wish to know from string theory: How hard is it to get flat enough potentials? Does embedding into string theory carry observational implications? How does reheating work? etc…
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String Phenomenology Workshop CERN 2008 String Inflation What might one hope to learn? about strings about inflation WMAP Seek: stringy inflationary signatures Because inflation is found in 4D effective theory, predictions tend to follow 4D mechanisms r 0.6 0.2 n s
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String Phenomenology Workshop CERN 2008 String Inflation What might one hope to learn? about strings about inflation WMAP Seek: stringy inflationary signatures Could hope that string inflation provides only a subset of the possible 4D inflationary possibilities. r 0.6 0.2 n s
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String Phenomenology Workshop CERN 2008 String Inflation What might one hope to learn? about strings about inflation WMAP Small-field models Hybrid models Large-field models r 0.6 0.2 n s
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String Phenomenology Workshop CERN 2008 String Inflation What might one hope to learn? about strings about inflation WMAP Small-field models Hybrid models Large-field models r 0.6 0.2 n s
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String Phenomenology Workshop CERN 2008 String Inflation What might one hope to learn? about strings about inflation WMAP Small-field models Hybrid models Large-field models r 0.6 0.2 n s
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String Phenomenology Workshop CERN 2008 String Inflation What might one hope to learn? about strings about inflation Linde & Kallosh Baumann & McAllister r 0.6 0.2 n s Strings: small tensor amplitude?
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String Phenomenology Workshop CERN 2008 String Inflation What might one hope to learn? about strings about inflation Lyth r 0.6 0.2 n s Strings: small tensor amplitude? Appears difficult to obtain large p
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String Phenomenology Workshop CERN 2008 Emerging Picture Mechanisms Robustness Mind broadening First attempts to get large field range: Type IIA: brane motion wrapped on a twisted torus. Type IIB: aperiodic B mn fields Silverstein & Westphal McAllister, Silverstein & Westphal
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String Phenomenology Workshop CERN 2008 Emerging Picture Mechanisms Robustness Mind broadening First attempts to get large field range: Type IIA: brane motion wrapped on a twisted torus. Type IIB:aperiodic B mn fields Silverstein & Westphal McAllister, Silverstein & Westphal Within the domain of low-energy effective theory?
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String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS
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String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Searches over the years for accelerating cosmologies in 4D and extraD supergravities lead instead to strong no-go results. Leading order in gs and a’ often give no-scale models for moduli (eg Kahler moduli in Type IIB). The flat potentials of no-scale models tend lie on the boundary of the no-go results; eg: Covi, Gomez-Reino, Gross, Louis, Palma & Scrucca (n=3 for no-scale models)
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String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Searches over the years for accelerating cosmologies in 4D and extraD supergravities lead instead to strong no-go results. Leading order in g s and ’ often give no-scale models for moduli (eg Kahler moduli in Type IIB). The flat potentials of no-scale models tend lie on the boundary of the no-go results Suggests looking for inflation starting with no-scale moduli but including subleading g s and ’ terms.
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String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS In 4D string loops and ’ corrections are suppressed (in Einstein frame) by powers of 6D volume, V -1/3. Becker, Becker, Haack & Louis
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String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Given several Kahler moduli, b » s, correction to K together with superpotential W = W 0 + A e a s can stabilize V at a very large volume minimum Balasubramanian, Berglund, Conlon & Quevedo Essentially any large volume is possible for a small range of s.
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String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Potential has naturally weak dependence on any other large moduli b » i » s with V ~ V( b, i ). If then up to 1/V and exp[-a i ] and exp[-a b ] terms Conlon & Quevedo
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String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Potential has naturally weak dependence on any other large moduli b » i » s with V ~ V( b, i ). If then up to 1/V and exp[-a i ] and exp[-a b ] terms Conlon & Quevedo
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String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Kahler modulus inflation: inflaton potential obtained by keeping terms that are of order exp[-a i ] Slow roll naturally arises when i is displaced to large values from its minimum. Conlon & Quevedo
![String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Kahler modulus inflation: inflaton potential obtained by keeping terms that are of order exp[-a i ] Slow roll naturally arises when i is displaced to large values from its minimum.](http://images.slideplayer.com./25/7994525/slides/slide_24.jpg "Conlon & Quevedo.")
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String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Fibre inflation: inflaton potential dominated by subleading 1/V ~ exp[-a s ] corrections rather than by exp[-a i ] corrections. Such corrections arise in the leading string loops, since U tree ~ V -3 while U loop ~ V -10/3. It turns out that such loops can also compete with the exp[-a i ] terms and so can ruin slow roll of Kahler Modulus Inflation. Cicoli, Conlon & Quevedo Cicoli, CB & Quevedo
![String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Fibre inflation: inflaton potential dominated by subleading 1/V ~ exp[-a s ] corrections rather than by exp[-a i ] corrections.](http://images.slideplayer.com./25/7994525/slides/slide_25.jpg "Such corrections arise in the leading string loops, since U tree ~ V -3 while U loop ~ V -10/3. It turns out that such loops can also compete with the exp[-a i ] terms and so can ruin slow roll of Kahler Modulus Inflation. Cicoli, Conlon & Quevedo Cicoli, CB & Quevedo.")
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String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS String loop potential: explicit 1-loop contributions have only been computed on orbifolded tori. Most of the potential’s complication lies in its dependence on the complex structure moduli. Dependence on Kahler moduli can be inferred using educated guesses based on kinds of loops that enter (KK tree exchange, loops of winding states, etc). Berg, Haack & Pajer Cicoli, Conlon & Quevedo
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String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS String loop potential: explicit 1-loop contributions have only been computed on orbifolded tori. Most of the potential’s complication lies in its dependence on the complex structure moduli. Dependence on Kahler moduli can be inferred using educated guesses based on kinds of loops that enter (KK tree exchange, loops of winding states, etc). Berg, Haack & Pajer Cicoli, Conlon & Quevedo Potentially dangerous terms drop from the potential!
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String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Kahler Modulus dependence of string loops: KK tree exchange Loop of winding states Berg, Haack & Pajer Cicoli, Conlon & Quevedo
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String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Kahler Modulus dependence of string loops: KK tree exchange Loop of winding states Berg, Haack & Pajer Cicoli, Conlon & Quevedo 2-cycle transverse to D7 2-cycle of intersecting D7s
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String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS A Specific Model: Choose a Calabi-Yau that is a K3 fibration plus a blow-up modulus, with 2 » 1 » 3 take leading corrections to W: add leading ’ and string loop corrections to K: Cicoli, CB & Quevedo
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String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Potential at leading order: stabilizes 3 ~ g s -1 and V ~ exp[a 3 ] Potential at next-to-leading order: acquire potential in 1 ~ exp[2 / 3] Natural slow roll once › 1, but boundary at ‹ 6.
![String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Potential at leading order: stabilizes 3 ~ g s -1 and V ~ exp[a 3 ] Potential at next-to-leading order: acquire potential in 1 ~ exp[2 / 3] Natural slow roll once › 1, but boundary at ‹ 6.](http://images.slideplayer.com./25/7994525/slides/slide_31.jpg "String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Potential at leading order: stabilizes 3 ~ g s -1 and V ~ exp[a 3 ] Potential at next-to-leading order: acquire potential in 1 ~ exp[2 / 3] Natural slow roll once › 1, but boundary at ‹ 6.")
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String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Potential at leading order: stabilizes 3 ~ g s -1 and V ~ exp[a 3 ] Potential at next-to-leading order: acquire potential in 1 ~ exp[2 / 3] Natural slow roll once › 1, but boundary at ‹ 6.
![String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Potential at leading order: stabilizes 3 ~ g s -1 and V ~ exp[a 3 ] Potential at next-to-leading order: acquire potential in 1 ~ exp[2 / 3] Natural slow roll once › 1, but boundary at ‹ 6.](http://images.slideplayer.com./25/7994525/slides/slide_32.jpg "String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Potential at leading order: stabilizes 3 ~ g s -1 and V ~ exp[a 3 ] Potential at next-to-leading order: acquire potential in 1 ~ exp[2 / 3] Natural slow roll once › 1, but boundary at ‹ 6.")
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String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Potential at leading order: stabilizes 3 ~ g s -1 and V ~ exp[a 3 ] Potential at next-to-leading order: acquire potential in 1 ~ exp[2 / 3] Natural slow roll once › 1, but boundary at ‹ 6. only one free parameter!
![String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Potential at leading order: stabilizes 3 ~ g s -1 and V ~ exp[a 3 ] Potential at next-to-leading order: acquire potential in 1 ~ exp[2 / 3] Natural slow roll once › 1, but boundary at ‹ 6.](http://images.slideplayer.com./25/7994525/slides/slide_33.jpg "only one free parameter!.")
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String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Higher loops? likely to introduce singularity at boundary ~ 6 guess: for O(1) coefficients, ratio of 2-loop to 1-loop terms is negligible when ‹ 5.9
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String Phenomenology Workshop CERN 2008 Fibre Inflation The Large Volume Scenario Inflation in the LVS Higher loops? likely to introduce singularity at boundary ~ 6 for O(1) coefficients, ratio of 2-loop to 1-loop terms is negligible when ‹ 5.9 Cicoli, CB & Quevedo
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String Phenomenology Workshop CERN 2008 Inflationary Observables Robust features More model dependent results
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String Phenomenology Workshop CERN 2008 Inflationary Observables Robust features More model dependent results Slow roll parameters depend only on N e
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String Phenomenology Workshop CERN 2008 Inflationary Observables Robust features More model dependent results Correlates r and n s like for large-field models.
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String Phenomenology Workshop CERN 2008 Inflationary Observables Robust features More model dependent results Correlates r and n s like for large-field models. Central value
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String Phenomenology Workshop CERN 2008 Inflationary Observables Robust features More model dependent results Getting large enough scalar perturbations requires volumes of order V ~ few thousand Never get much more than 50-60 e-foldings, so might expect to see imprints of onset of inflation at horizone exit. Slowness of roll does not require tuning of parameters in the potential, but does require initial conditions relatively near to the edge of the Kahler cone
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String Phenomenology Workshop CERN 2008 Summary Systematic large volume expansions seem able to provide slow roll regimes with less tuning than most inflationary scenarios. Fibre inflation models can allow trans- Planckian excursions of the inflaton, and so can accommodate observably large r
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String Phenomenology Workshop CERN 2008 Many thanks to the Organizers!! Angel Uranga The TH administrative staff (Nanie, Nadje & Jean) Ignatio Antoniadis Elias Kiritsis Fernando Quevedo Herman Verlinde
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String Phenomenology Workshop CERN 2008 fin
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