From String Theory to the LHC via No-Scale Inflation John Ellis 13.8 Billion Years 10 28 cm Today...
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Transcript of From String Theory to the LHC via No-Scale Inflation John Ellis 13.8 Billion Years 10 28 cm Today...
![Page 1: From String Theory to the LHC via No-Scale Inflation John Ellis 13.8 Billion Years 10 28 cm Today Big Bang What happened here? And the connection with.](https://reader030.fdocuments.net/reader030/viewer/2022012922/56649d9e5503460f94a89388/html5/thumbnails/1.jpg)
From String Theory to the LHC
via No-Scale Inflation
John Ellis
13.8 Billion Years
1028 cmToday
Big Bang
What
happened here?
And the connection
with here?
![Page 2: From String Theory to the LHC via No-Scale Inflation John Ellis 13.8 Billion Years 10 28 cm Today Big Bang What happened here? And the connection with.](https://reader030.fdocuments.net/reader030/viewer/2022012922/56649d9e5503460f94a89388/html5/thumbnails/2.jpg)
Cosmological Inflation in Light of Planck
A scalar in the sky? Supersymmetry/supergravity?
![Page 3: From String Theory to the LHC via No-Scale Inflation John Ellis 13.8 Billion Years 10 28 cm Today Big Bang What happened here? And the connection with.](https://reader030.fdocuments.net/reader030/viewer/2022012922/56649d9e5503460f94a89388/html5/thumbnails/3.jpg)
The Spectrum of Fluctuations in the Cosmic Microwave Background
The position of the first peak
total density ΩTot
The other peaks
depend on density of
ordinary matter Ωatoms
& dark matter ΩDark
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Cosmological Inflation in Light of BICEP2
Quantum gravity radiation in the sky?
![Page 5: From String Theory to the LHC via No-Scale Inflation John Ellis 13.8 Billion Years 10 28 cm Today Big Bang What happened here? And the connection with.](https://reader030.fdocuments.net/reader030/viewer/2022012922/56649d9e5503460f94a89388/html5/thumbnails/5.jpg)
Planck sees Polarized Dust
BICEP2 claim crumbles into dust
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Some Big Questions
• Why is the Universe so big and old?• Why is it (almost) homogeneous on large
scales?• Why is its geometry (almost) Euclidean?• What is the origin of structures in the Universe?
A possible answer:
Cosmological inflation• What do the data tell us?• Models of inflation
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Primordial Perturbations
• “Cosmological constant” due to vacuum energy in “inflaton” field ϕ: Λ ~ V(ϕ) ≠ 0
• Quantum fluctuations in ϕ cause perturbations in energy density (scalar) and metric (tensor)
• (Almost) independent of scale size
• Visible in cosmic microwave background (CMB)
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Inflationary Perturbations in a Nutshell
• Universe expanding like de Sitter• Horizon information loss mixed state• Effective ‘Hawking temperature’ H/2π• Expect quantum fluctuations:
<ϕϕ>, <hh> ~ H2
(inflaton, gravitational field: gμν = ημν + hμν) Scalar (density), tensor perturbations• Should have thermal spectrum• Scalars enhanced by evolution of ϕ r ~ ε
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Slow-Roll Inflation• Expansion driven by cosmological constant:
• Getting small density perturbations requires a “small” potential:
• That is almost flat: , small
so as to get sufficient e-folds of expansion:
• Main observables of scalar and tensor pert’ns:• Scalar tilt: , tensor/scalar ratio:• Perturbations ~ Gaussian: look for deviation (fNL)
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Planck +
other data
Starobinsky
R + R2 model
ϕ2
ϕϕ2/3
Inflationary LandscapeMonomial
Single-field
potentials
ϕ3
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• Links to low-energy physics?– Only SM candidate for inflaton is Higgs
• BUT negative potential, ….
• Link to other physics?–SUSY partner of RH (singlet) neutrino?–Some sort of axion?
• Links to Planck-scale physics?– Inflaton candidates in string theory?– Inflaton candidates in compactified string models?
Challenges for Inflationary Models
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Inflationary Models in Light of Planck
• Planck CMB observations consistent with inflation• Tilted scalar perturbation spectrum (rolling down):
ns = 0.958 ± 0.006
• BUT strengthen upper limit on tensor perturbations: r < 0.12
• Challenge for many simple
inflationary models• Starobinsky R2 to rescue?• Higgs/Supersymmetry/supergravity to rescue?
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Starobinsky Model• Non-minimal general relativity (singularity-free
cosmology):• No scalar!?• Inflationary interpretation, calculation of
perturbations:
• Conformally equivalent to scalar field model:
Starobinsky, 1980
Mukhanov & Chibisov, 1981
Stelle; Whitt, 1984
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Higgs Inflation: a Single Scalar?
• Standard Model with non-minimal coupling to gravity:
• Consider case : in Einstein frame
• With potential:Similar to Starobinsky, but not identical
• Successful inflationary potential at
Bezrukov & Shaposhnikov, arXiv:0710.3755
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Higgs Inflation: a Single Scalar?• Successful inflation for
• BUT:– Requires λ > 0 beyond MP: need MH > 127 GeV?
– How natural is such a large value of ξ? Unitarity?
Bezrukov & Shaposhnikov, arXiv:0710.3755
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Theoretical Constraints on Higgs Mass
• Large Mh → large self-coupling → blow up at low-energy scale Λ due to renormalization
• Small: renormalization due to t quark drives quartic coupling < 0at some scale Λ→ vacuum unstable
• Vacuum could be stabilized by SupersymmetryDegrassi, Di Vita, Elias-Miro, Giudice, Isodori & Strumia, arXiv:1205.6497
Instability @
1011.1±1.1 GeV
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Inflation Cries out for Supersymmetry
• Want “elementary” scalar field
(at least looks elementary at energies << MP)
• To get right magnitude of perturbations
prefer mass << MP
(~ 1013 GeV in simple φ2 models)• And/or prefer small self-coupling λ << 1• Both technically natural with supersymmetry
JE, Nanopoulos, Olive, & Tamvakis: 1983
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Sneutrino Inflation?
• See-saw model of neutrino masses requires massive singlet (right-handed) neutrinos
• In supersymmetric models would be accompanied by massive sneutrinos, with m2ϕ2 potential
• Decay of sneutrino inflaton
gives efficient leptogenesis• Disfavoured by Planck?
– Not necessarily …• Multiple sneutrinos …
• Different trajectories for different v
JE, Raidal & Yanagida: hep-ph/0303242
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From Supersymmetry to Supergravity
• The only good symmetry is a local symmetry
(cf, gauge symmetry in Standard Model)• Local supersymmetry = supergravity• Early Universe cosmology needs gravity• Supersymmetry + gravity = supergravity• Superpartner of graviton is gravitino fermion• Gravitino condensation? (cf, quarks in QCD)• Mechanism for inflation?
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No-Scale Supergravity Inflation
• Supersymmetry + gravity = Supergravity• Include conventional matter?• Potentials in generic supergravity models have
‘holes’ with depths ~ – MP4
• Exception: no-scale supergravity• Appears in compactifications of string• Flat directions, scalar potential ~ global model +
controlled corrections JE, Nanopoulos & Olive, arXiv:1305.1247, 1307.3537
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First No-Scale Supergravity Model of Inflation
• No ‘holes’ in effective potential with negative cosmological constant
JE, Enqvist, Nanopoulos, Olive & Srednicki, 1984
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No-Scale Supergravity Inflation Revived
• Simplest SU(2,1)/U(1) example:• Kähler potential:• Wess-Zumino superpotential:• Assume modulus T = c/2 fixed by ‘string
dynamics’• Effective Lagrangian for inflaton:
:• Modifications to globally supersymmetric case• Good inflation possible … JE, Nanopoulos & Olive, arXiv:1305.1247
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No-Scale Supergravity Inflation
• Inflationary potential for
JE, Nanopoulos & Olive, arXiv:1305.1247
Special case = Starobinsky
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If it looks and smells like Starobinsky …
• Starobinsky model:
• After conformal transformation:
• Effective potential:• Identical with the no-scale Wess-Zumino model
for the case
… it actually IS StarobinskyJE, Nanopoulos & Olive, arXiv:1305.1247
Is there more profound connection?
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Beyond Starobinsky• Exponential
approach to constant potential:
• Relations between observables:
• E.g., multiple no-scale moduli:
• Characteristic of generic string compactifications
• Tensor/scalar ratio may be < prediction of
Starobinsky
model:
• String phenomenology via the CMB?
JE, Nanopoulos & Olive, arXiv:1307.3537
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See also …
• Nakayama, Takahashi & Yanagida – arXiv:1305.5099• Kallosh & Linde – arXiv:1306:3214• Buchmuller, Domcke & Kamada – arXiv:1306.3471• Kallosh & Linde – arXiv:1306.5220• Farakos, Kehagias and Riotto – arXiv:1307.1137• Roest, Scalisi & Zavala – arXiv:1307.4343• Kiritsis – arXiv:1307.5873• Ferrara, Kallosh, Linde & Porrati – arXiv:1307.7696• …
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• Grand Unification within SU(5)• Embed in no-scale supergravity• Inflation via a combination of 5, 5* Higgs fields• Avoids the problems of the original Higgs inflation
model: potential positive• Interpolates between
the Starobinsky model
(Planck) and a quadratic
potential (BICEP2)
New Higgs Inflation in No-Scale SUSY GUT
JE, He & Xianyu, arXiv:1411.5537
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• A no-scale supergravity model of inflation that interpolates between Planck and BICEP2:
• Identify inflaton with components of modulus T:
• Effective Lagrangian:
A No-Scale Inflationary Model to Fit Them All
JE, García, Nanopoulos & Olive, arXiv:1405.0271
Starobinsky Quadratic
Motivated by orbifold compactification
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A No-Scale Inflationary Model to Fit Them All
JE, García, Nanopoulos & Olive, arXiv:1405.0271
Starobinsky
Quadratic
Starobinsky
+ term to fix direction
in complex T plane
![Page 30: From String Theory to the LHC via No-Scale Inflation John Ellis 13.8 Billion Years 10 28 cm Today Big Bang What happened here? And the connection with.](https://reader030.fdocuments.net/reader030/viewer/2022012922/56649d9e5503460f94a89388/html5/thumbnails/30.jpg)
A No-Scale Inflationary Model to Fit Them All
JE, García, Nanopoulos & Olive, arXiv:1405.0271
Quadratic limit
Starobinsky limit
Circling the drain
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• Starting angle interpolates between limits
A No-Scale Inflationary Model to Fit Them All
JE, García, Nanopoulos & Olive, arXiv:1405.0271
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• Predictions for general initial conditions• ns, r as functions of initial values
• Time will tell what Nature has chosen!
A No-Scale Inflationary Model to Fit Them All
JE, García, Nanopoulos & Olive, arXiv:1405.0271
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• Isocurvature effects on curvature perturbations may suppress tensor/scalar ratio r
• ns, r, non-Gaussianity dependences on initial values
Two-Field Analysis ofNo-Scale Inflationary Model
JE, García, Nanopoulos & Olive, arXiv:1409.8197
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How many e-Folds of Inflation?• General expression:
• In no-scale supergravity models: Amplitude of
perturbations
Equation of state
during inflaton decay
Inflaton
decay rate
JE, García, Nanopoulos & Olive, in preparation
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How many e-Folds of Inflation?
• Dependence on inflaton decay rate of density after reheating
• Dependence on inflaton decay rate of effective equation of state
JE, García, Nanopoulos & Olive, in preparation
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Inflaton Decays in No-Scale Models
• Two-body decay in sneutrino inflation:• Three-body decays in no-scale:
• Decays into vector bosons:
• Connection with
sparticle masses• How do data constrain models?
JE, García, Nanopoulos & Olive, in preparation
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Planck Constraints on # of e-Folds
JE, García, Nanopoulos & Olive, in preparation
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Planck Constraints on # of e-Folds
JE, García, Nanopoulos & Olive, in preparation
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No-Scale Framework for Particle Physics & Dark Matter
• Incorporating LHC constraints, Higgs mass, flavour, supersymmetric dark matter, Starobinsky-like inflation, leptogenesis, neutrino masses, …
JE, Nanopoulos & Olive, arXiv:1310.4770
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No-Scale Framework for Particle Physics & Dark Matter
• Incorporating LHC constraints, Higgs mass, flavour, supersymmetric dark matter, Starobinsky-like inflation, leptogenesis, neutrino masses, …
JE, Nanopoulos & Olive, arXiv:1310.4770
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Summary• Inflation may solve some of the biggest problems in
cosmology: age, size, homogeneity, flatness, …• Open season for building inflationary models• Inflation cries out for supersymmetry• Cosmology requires supergravity• Natural framework: no-scale supergravity• Derived from string theory• CMB data can constrain models of particle physics• Will the LHC discover supersymmetry?