SCENARIO AND COSMOLOGY F. Quevedo, Cambridge/CERN. Zurich RTN - - PowerPoint PPT Presentation

▶
scenario and
SMART_READER_LITE
LIVE PREVIEW

SCENARIO AND COSMOLOGY F. Quevedo, Cambridge/CERN. Zurich RTN - - PowerPoint PPT Presentation

Sep 06, 2023 214 likes •717 views

LARGE VOLUME STRING SCENARIO AND COSMOLOGY F. Quevedo, Cambridge/CERN. Zurich RTN September 2009. J. Conlon, FQ hep-th/0509012 M. Cicoli, J. Conlon, FQ, 0805.1029[hep-th] J. Conlon, R. Kallosh, A. Linde, FQ, arXiv:0806.0809 [hep-th] M.

slide-1
SLIDE 1

LARGE VOLUME STRING SCENARIO AND COSMOLOGY

  • F. Quevedo, Cambridge/CERN. Zurich RTN September 2009.
  • J. Conlon, FQ hep-th/0509012
  • M. Cicoli, J. Conlon, FQ, 0805.1029[hep-th]
  • J. Conlon, R. Kallosh, A. Linde, FQ, arXiv:0806.0809 [hep-th]
  • M. Cicoli, C. Burgess, FQ arXiv:0808.0691[hep-th].

J.P. Conlon, A. Maharana, FQ arXiv:0810.5660 [hep-th]

  • S. Krippendorf, FQ arXiv:0901.0683 [hep-th]

R.Blumenhagen, J. Conlon, S. Krippendorf, S. Moster, FQ arXiv:0906.3297 [hep-th]

slide-2
SLIDE 2

STRING PHENOMENOLOGY/ COSMOLOGY

slide-3
SLIDE 3

Phenomenology String Theory String Phenomenology

slide-4
SLIDE 4

THE LHC IS COMING!

slide-5
SLIDE 5

DISCOVERIES BSM?

  • Nothing
  • Low-energy SUSY
  • Large extra dimensions
  • Technicolor/Warping
  • New Higgses, generations, Z’s, W’s, etc
  • All of the above
  • None of the above
  • ….
slide-6
SLIDE 6

COSMOLOGY vs LOW-ENERGY SUSY

  • GOOD:

► Cold Dark Matter (in some models, need R-parity)

  • BAD:

► Gravitino problem, ► Cosmological moduli problem, ► Thermal destabilisation, ► Overshooting, ► Gravitino mass, ► eta-problem, scale of inflation,…

slide-7
SLIDE 7

String Model Building:

  • Global Models (e.g. Heterotic)
  • Local Brane Models (e.g. IIB)
slide-8
SLIDE 8

Bottom-up Approach

  • Gauge group
  • Chiral spectrum
  • Yukawa couplings
  • Gauge couplings
  • Proton stability
  • Flavour symmetries
  • Moduli Stabilisation
  • Cosmological constant
  • SUSY Breaking
  • Scales (unification,

axions,…)

  • Inflation, Reheating
  • Cosmological moduli

problem Local (brane) issues Global (bulk) issues

Aldazabal,Ibanez, FQ, Uranga 2000

slide-9
SLIDE 9

Model Degeneracy (IIB)

  • Choice of closed string backgrounds:

gmn (Calabi-Yaus), Fluxes H3, F3; F5 (fix U, S; warping, 10500 landscape)

  • Open string sector: Brane set-up

Hidden Sector: number of D7 branes; E3 branes, gaugino condensation SM sector: magnetised D7 (F2 background), D3 at singularity (choice of singularities)

slide-10
SLIDE 10

GLOBAL ISSUES

slide-11
SLIDE 11

MODULI STABILISATION

4-cycle size: τ (Kahler moduli) 3-cycle size: U (Complex structure moduli) + String Dilaton: S

slide-12
SLIDE 12

LARGE Volume Scenario

slide-13
SLIDE 13

Perturbative vs Non perturbative :

  • In general:
  • Then:
  • Usually V0 dominates but

V0=0 (no-scale )

  • Dominant term is VJ unless

W0<<1 (e.g. KKLT)

slide-14
SLIDE 14

Exponentially Large Volumes

Example :

BBCQ, CQS (2005)

Exponentially large volumen + Broken SUSY!!!

Fluxes

Volume

Perturbative (alpha’) corrections to K Nonperturbative corrections to W

slide-15
SLIDE 15

KKLT SUSY AdS

Large volume Non-SUSY AdS W0~10-10 W0<10-11 Both minima close

For de Sitter: Anti D3 Branes (KKLT) D-terms (BKQ, …, CGQS, KQ)

slide-16
SLIDE 16

e.g.Hidden sector W chiral matter

(Or W~ φ1φ2e-aT2 ) LARGE volume de Sitter!

  • S. Krippendorf, FQ 2009
slide-17
SLIDE 17

General Conditions for LARGE Volume

  • h12 > h11 > 1
  • At least one blow-up mode (point-like singularity)
  • Blow-up mode fixed by non-perturbative effects,

volume by alpha’ corrections

  • For Nsmall blow-up modes, there are L=h11-Nsmall-1

flat directions at tree-level

  • These directions are usually lifted by perturbative

string effects

Cicoli, Conlon, FQ

slide-18
SLIDE 18

Swiss Cheese Calabi-Yau’s

e.g.

Blumenhagen, et al., Grimm et al., Kreuzer et al. 08

But also K3 fibrations, etc.

slide-19
SLIDE 19

Relevant Scales

  • String scale Ms=MP/V 1/2
  • Kaluza-Klein scale MKK=MP/V 2/3
  • Gravitino mass m3/2=W0 MP/V
slide-20
SLIDE 20

General Scenarios (before 2009)

  • MString = MGUT~ 1016 GeV (V~104-5)
  • W0~10-11<<1 (or W0~1 plus warping)
  • Fits with coupling unification
  • Natural scale of most (all?) string inflation models.
  • Axi-volume quintessence scale (w=-0.999….)
  • Cosmological moduli problem!
  • MString = Mint.~ 1012 GeV (V~1015)
  • W0~1 (no tuning here)
  • m3/2~1 TeV
  • QCD axion scale
  • Neutrino masses LLHH
  • Cosmological moduli problem
  • MString = 1 TeV

(V~1030)

  • W0~1
  • Most exciting, but 5th Force (volume modulus m~10-15 eV)??
slide-21
SLIDE 21

INFLATION

slide-22
SLIDE 22

String Inflation Motivation

  • Inflation: very successful but is only

ad-hoc scenario in search of a theory

  • String theory: fundamental theory but

lacks experimental tests.

  • Is it possible to ‘derive’ inflation from

string theory?

slide-23
SLIDE 23

Need to compute scalar potential from String theory satisfying slow- roll conditions:

Number of e-folds N>50 Density perturbations

(r=16 ε )

slide-24
SLIDE 24

Two General Classes of String Inflation

  • Open String Inflaton
  • Closed String Inflaton
slide-25
SLIDE 25

OPEN STRING INFLATON

e.g. BRANE - ANTIBRANE INFLATION

Branes inflate while two approach Slow-roll or DBI (need tuning but tunable, r~0,Tachyon

condensation:~hybrid inflation + cosmic strings)

Also D3/D7, Wilson-line

Dvali+Tye BMQRZ Dvali, Shafi, Solganik KKLMT

slide-26
SLIDE 26

CLOSED STRING INFLATON

Dilaton, Complex Structure

  • r Kahler Modulus:
  • Axion Inflaton
  • Blow-up modulus inflaton
  • Fibre inflaton
  • Volume
slide-27
SLIDE 27

KAHLER INFLATONS

  • Blow-up modes
  • Fibration modes
  • Volume modulus
slide-28
SLIDE 28

Kähler Moduli Inflation (Blow-up)

Calabi-Yau: h21>h11>2

volume

τn V

Conlon-FQ Bond et al. …

Small field inflation (r<<<1) 105<Volume<107 No fine-tuning!! 0.960<n<0.967 Loop corrections??

~

slide-29
SLIDE 29

V

Fibre Inflation

slide-30
SLIDE 30

Ne ns ns r r Observable gravity waves ! (can be ruled out by Planck if they

  • bserve them and CMBpol… if

they do not observe them) No tuning but initial conditions close to bdry of Kahler cone

slide-31
SLIDE 31

LOCAL ISSUES

slide-32
SLIDE 32

LARGE Volume Implies

Standard Model is localised !

( SM D7 cannot wrap the exponentially large cycle since g2=1/V2/3 )

  • Fractional D3/D7 Brane at a singularity

(collapsed cycle)

  • Magnetised D7 - Brane wrapping a `small’ four-cycle
  • Local F-Theory

Blumenhagen et al. 08 Donagi, Wijnholt; Vafa et al. 08

slide-33
SLIDE 33

Modular Model Building

(Bottom up approach)

Aldazabal,Ibanez, FQ, Uranga 2000 Verlinde,Wijnholt 2006, Vafa et al 08

slide-34
SLIDE 34

Universe D3 Brane

  • r

D7 Brane

slide-35
SLIDE 35

Standard Model at (Fractional) D3/D7 Branes at Singularities

Collapsing single 4-cycle: del Pezzo surfaces dPn, n=0,1, …,8 (P2 blown-up at n arbitrary points c1>0, b2=n+1, 2n-8 parameters, n>3) More general singularities, e.g. Ypq, Labc

slide-36
SLIDE 36

Simple Singularities/Quivers

e.g. del Pezzo 0 = C3/Z3 ni D3 Branes (group ПU(ni)) mj D7 Branes (group ПU(mi)) Arrows=bi-fundamentals W=closed arrows loop

(=0 in smooth P2, Conlon, Maharana, FQ)

Anomaly/tadpole cancellation `Hypercharge’ (ni≠nj) 3 Families! Douglas,Moore; Hanany; Uranga et al

slide-37
SLIDE 37

Standard Models LR-Symmetric Models Pati-Salam Models Trinification Models

slide-38
SLIDE 38

Problem for dP0: Yukawa couplings

E-values (M,M,0). From global flavour symmetry SU(3) (?)

Del Pezzo1 Singularity

SU(2)xU(1) Flavour symmetry Conlon, Maharana, FQ Hierarchy in 3 generation masses!!!! Higgsing gives back dP0!!!

slide-39
SLIDE 39

e.g. Realistic dP1 Models

Standard Model LR Symmetric Model

slide-40
SLIDE 40

Higher del Pezzos

Triplication of families very limited In general most quivers k<4 arrows

For dP8 model, see H.Verlinde, M.Wijnholt (+Buican, Malyshev, Morrison) 06,07

slide-41
SLIDE 41

LOCAL/GLOBAL MIXING

slide-42
SLIDE 42

Local/Global Mixing

  • Standard Model in small cycle
  • SM cycle NOT fixed by non-perturbative

effects:

  • SM chiral implies: W=

MSSM: <Φ>=0, so W=0, (singularity)? Or <|Φ|2>= Blumenhagen et al. FSM=KTSM W=0

  • r FSM≠0
slide-43
SLIDE 43

Towards a Compact Model

  • h21>h11>3 (e.g. h+

11=3, h- 11=1)

  • At least one blow-up
  • Tadpole cancellation (D7s, Fluxes)
slide-44
SLIDE 44

Generic Features

  • Aproximate Flavour Symmetries
  • Hyperweak Interactions

(SM fields charged under D7 gauge interactions g2=1/V2/3 <<<1, CDF?)

Burgess et al. 2008 Conlon, Maharana, FQ

(Approximate isometries)

slide-45
SLIDE 45

SUSY Breaking

  • Approximate Universality
  • Two cases: FSM≠0 soft terms~m3/2~1/V

FSM=0 soft terms <<m3/2 Δm~1/V2 ~m2

3/2/Mplanck

CAQS, Conlon (Mirror Mediation)

slide-46
SLIDE 46

Phenomenology vs Cosmology!

  • Low scale inflation?
  • Volume Inflation?

Conlon, Kallosh, Linde, FQ

Gravitino mass 1 TeV/Gravitino mass >> 1 TeV ?? (string scale 1011 GeV/ string scale ~ GUT scale)

slide-47
SLIDE 47

New Scenario FSM=0

  • Ms~Mp/V1/2, MKK~Mp/V2/3
  • M3/2~Mp/V (no gravitino problem)
  • Δm>Mp/V2~1TeV (smallest volume V~106)
  • Lightest modulus m~Mp/V3/2 (no CMP!)
  • String/KK scales closer to standard inflation scale
  • MGUT~MsV1/6~1016 GeV (GUT scale and solves

hierarchy problem!)

  • Other contributions to SUSY breaking?

Blumenhagen, Conlon, Krippendorf, Moser, FQ

slide-48
SLIDE 48

Conclusions

  • Continuous progress in this `Decade of Applied String Theory’
  • Bottom-up (Local Model Building) fits with Large Volume
  • Realistic models at singularities: powerful quiver/dimer constructions

(Modular road towards the stringy SM)

  • General features (hyperweak interactions, approximate flavour

symmetries, massive U(1)’s)

  • Realistic cosmology (Models of inflation, no CMP, etc.)
  • Open challenges (compact CY, detailed susy breaking, gauge

unification(?), EFT in F-theory models, (compact CY, detailed susy breaking, (p)reheating (see Barnaby, Bond, Kofman Friday’s paper) )

slide-49
SLIDE 49