Sneutrino Cold Dark Matter, Oxford

Thermal Sneutrino Dark Matter Thermal Sneutrino Dark Matter in the in the FFDD-Term Model of Hybrid Inflation-Term Model of Hybrid Inflation

The

Uni

vers

ity

of M

anch

este

r

Frank [email protected]

University of Manchester

in collaboration with A. Pilaftsis

FFD, A. Pilaftsis, JHEP 0810 (2008) 080

Particle Physics Seminar Oxford, 7 May 2009

7/5/2009Frank Deppisch Sneutrino Dark Matter in the F(D) Term Model22/40/40

OverviewOverview

IntroductionDark Matter EvidenceSupersymmetryNeutrino Physics

FD Term Hybrid ModelSuperpotentialInflaton VEVHybrid Inflation

RH Sneutrino Dark MatterMass Spectrum

Annihilation

Conclusion


Evidence for Dark MatterEvidence for Dark Matter

Cluster FormationGalactic Rotation CurvesGravitational LensingCMB FluctuationsLarge Scale StructureStandard Cosmological Model:

Cold Dark Matter Component of the Universe

CDM h2≈0.11


SupersymmetrySupersymmetryMSSM: Minimal extension of the Standard Model with two Higgs doublets and conserved R-parity

http://www.physics.gla.ac.uk/ppt/susy.htm


SupersymmetrySupersymmetryMSSM: Minimal extension of the Standard Model with two Higgs doublets and conserved R-parity

SUSY must be broken⇒ In general: Introduction of more than 100 free parameters⇒ Required: Theoretical framework for SUSY breaking⇒ Minimal Supergravity (mSUGRA), Universality at GUT Scale

http://www.physics.gla.ac.uk/ppt/susy.htm


Neutrino Oscillations⇒ Mixing angles and mass differences

Absolute Mass Scale

NeutrinosNeutrinos

sin212=0.30−0.050.04 ,sin223=0.50−0.12

0.14 ,sin2130.028m12

2 =8.1−0.60.6⋅10−5 eV2 ,m13

2 =±2.2−0.50.7⋅10−3 eV2

m10.5eV


Neutrino Oscillations⇒ Mixing angles and mass differences

Absolute Mass Scale

Seesaw Mechanism⇒ Add heavy right-handed neutrinos

But: With suitable flavor symmetry in MR and mD, right-handed neutrinos can be as light as 100 GeV

NeutrinosNeutrinos

sin212=0.30−0.050.04 ,sin223=0.50−0.12

0.14 ,sin2130.028m12

2 =8.1−0.60.6⋅10−5 eV2 ,m13

2 =±2.2−0.50.7⋅10−3 eV2

m10.5eV

0 mDT

mD M R ⇒ m≈0.1eV mD

100GeV 2

M R

1014GeV −1


FFDD-Term Hybrid Model-Term Hybrid Model

Extension of the MSSMW=W MSSM=0

Garbrecht, Pallis, Pilaftsis '06Garbrecht, Pallis, Pilaftsis '06

A Minimal Particle-Cosmology Supersymmetric Model



Extension of the MSSMInflaton-Waterfall sector

W=W MSSM=0

S X 1X 2−M 2






Effective µ term, µ = λ ⟨S⟩

W=W MSSM=0

S X 1X 2−M 2

S H uH d






Effective µ term, µ = λ ⟨S⟩Effective neutrino Majorana mass, M = ρ ⟨S⟩Neutrino Yukawa coupling

W=W MSSM=0

S X 1X 2−M 2

S H uH d

ij

2S N i

N j

hij Li

H uN j






Effective µ term, µ = λ ⟨S⟩Effective neutrino Majorana mass, M = ρ ⟨S⟩Neutrino Yukawa coupling

Fayet-Iliopoulos D-Term

W=W MSSM=0

S X 1X 2−M 2

S H uH d

ij

2S N i

N j

hij Li

H uN j

−g X

2mFI

2 D X




Inflaton VEVInflaton VEV

Soft SUSY breaking Lagrangian

−Lsoft⊃M S2 S∗ SM N

2 N i∗ N i A S X 1 X 2 AS H u H d

ij

2A S N i

N j−a S M 2 S




Scalar Potential ( ⟨X1,2⟩ = M )



ij

2A S N i

N j−a S M 2 S

V S≈∣ S ⟨X 1⟩∣2∣S ⟨X 2⟩∣

2M S2 S∗ S[M 2A−aS Sh.c.]

=22 M 2M S2 S∗ S[M 2 A−aS Sh.c. ]





Inflaton VEV (κ ≈ λ ≈ ρ ≈ 10−2)



ij

2A S N i

N j−a S M 2 S

V S≈∣ S ⟨X 1⟩∣2∣S ⟨X 2⟩∣


=22 M 2M S2 S∗ S[M 2 A−aS Sh.c. ]

⟨S ⟩= 12∣A−aS∣O M SUSY

2 /M ≈102 M SUSY





Inflaton VEV (κ ≈ λ ≈ ρ ≈ 10−2)



ij

2A S N i

N j−a S M 2 S

V S≈∣ S ⟨X 1⟩∣2∣S ⟨X 2⟩∣


=22 M 2M S2 S∗ S[M 2 A−aS Sh.c. ]

⟨S ⟩= 12∣A−aS∣O M SUSY

2 /M ≈102 M SUSY

=⟨S ⟩≈M SUSY

µ-Parametermij

N=ij ⟨S ⟩≈M SUSY

Majorana Mass Matrix


FFDD-Term Hybrid Inflation-Term Hybrid Inflation

Hybrid Inflation (Linde '91)

New scalar field ends inflation by acquiring VEV





F-Term Hybrid Inflation(Copeland et al., Dvali, Shafi, Schaefer '94)

Waterfall Fields X1, X2

Scalar Potential from F terms and supergravity/loop corrections

W= S X 1X 2−M 2





F-Term Hybrid Inflation(Copeland et al., Dvali, Shafi, Schaefer '94)

Waterfall Fields X1, X2

Scalar Potential from F terms and supergravity/loop corrections

FD-Term Hybrid Inflation (Garbrecht, Pilaftsis '06)

Subdominant non-anomalous FI D-term breaking discrete D-parity in waterfall sectorU(1)X gauge sector fields can decay ⇒ entropy release ⇒ avoid gravitino overabundance problem

W= S X 1X 2−M 2


Constraints from InflationConstraints from Inflation

Bounds on model parameters κ, λ, ρ fromNumber of e-folds

Power spectrum of curvature perturbations

Spectral index

N e=1

mPl2 ∫end

exit

d V inf

V inf' ≈55

P R1/2= 1

23mPl

V inf3/2exit

V inf' exit

≈4.86⋅10−5

ns−1=2mPl2 V inf

' ' exitV inf exit

=−0.037−0.0150.014


Constraints from InflationConstraints from Inflation

Spectral Index

Slow-roll slope from SUGRA and radiative corrections

≈≈23.2⋅10−2⇒ At inflationary scale M≈1016 GeV for minimal (next-to-minimal) Kähler potential

≈≈1.11.8⋅10−2⇒ At EW scale

RG Evolution


Sneutrino Mass SpectrumSneutrino Mass Spectrum

FD-Term Model conserves R-parity → LSP is stable


Sneutrino Mass SpectrumSneutrino Mass Spectrum

FD-Term Model conserves R-parity → LSP is stableRight-Handed Sneutrino Mass Matrix(small Yukawa interactions with LH sneutrinos neglected)

→ 3 Heavy and 3 Light Right-Handed Sneutrinos

→ Lightest Right-Handed Sneutrino can be LSP

N 1,2,3 , N 1,2,3∗ T 2 vS

2M N2 Avu vd

A∗vu vd 2 vS

2M N2 N 1,2,3

N 1,2,3∗

m N LSP

2 =2 vS2M N

2 −∣ AvSvu vd∣

≈2m02−∣A0∣, mSUGRA, tan ≫1,=≪1


Right-Handed Sneutrino LSP Right-Handed Sneutrino LSP Scan over mSUGRA parameters (A0 = 300 GeV, µ > 0, tanβ = 10,30)

Sneutrino LSP points to low-energy SUSY spectrum, consistent with annihilation via Higgs m N 1

≈20−100 GeV


Sneutrino Cold Dark MatterSneutrino Cold Dark Matter

MSSM (+ RH Neutrinos)Left-Handed Sneutrino LSP

Annihilates too efficiently (gauge interaction)





Right-Handed Sneutrino LSPOvercloses Universe as thermal DM (small Yukawa interaction)

Possible as non-thermal DM (Gopalakrishna, de Gouvêa, Porod '06)







Left-Right Mixtures possible (Arina, Fornengo '06)







Left-Right Mixtures possible (Arina, Fornengo '06)

FD-Term Model → New Interaction12 N i

∗ N i∗H u H dh.c. F S=

12 N i

N i H uH dfrom inflaton F-term

Quartic Coupling to Higgs Fields (McDonald '94, Burgess et al. '01)


Annihilation ChannelsAnnihilation Channels

12


Dark Matter SearchesDark Matter Searches

Direct SearchesElastic Scattering between Sneutrino and Nucleus

via t-channel Higgs exchangePer Nucleon

Experiments: CDMS-II, SuperCDMS, Xenon1T

elnucleon≈5⋅10−50 cm2 10−4

2

100GeVmH 1

4

50GeVm N 1

2


Dark Matter SearchesDark Matter Searches

Direct SearchesElastic Scattering between Sneutrino and Nucleus

via t-channel Higgs exchangePer Nucleon

Experiments: CDMS-II, SuperCDMS, Xenon1T

Indirect SearchesDetection of Dark Matter annihilation products

such as photons, positrons, anti-protonsHigh-energy Neutrinos from Sun and Earth

elnucleon≈5⋅10−50 cm2 10−4

2

100GeVmH 1

4

50GeVm N 1

2


Sneutrino AnnihilationSneutrino Annihilation

Calculation of Sneutrino Relic Density

Higgs properties calculated using CPSuperH (Lee at al. '03)

Annihilation via Higgs

Inflationary Bounds

Direct WIMP Searches

DM h2=0.11

Scenario I: m0=70 GeV, m1/2=243 GeV, A0=300 GeV, tanβ =10, µ =303 GeV

m N 1≈mH 1

/22⋅10−4

2.35.8⋅10−4

≈10−1...−3



Scenario II: m0=125 GeV, m1/2=212 GeV, A0=300 GeV, tanβ =30, µ =263 GeV

DM h2=0.11




Inflationary Bounds


m N 1≈mH 1

/22⋅10−4

2.35.8⋅10−4

≈10−1...−3



Scenario II: m0=125 GeV, m1/2=212 GeV, A0=300 GeV, tanβ =30, µ =263 GeV

DM h2=0.11




Inflationary Bounds


m N 1≈mH 1

/22⋅10−4

2.35.8⋅10−4

≈10−1...−3

H ere be H umans


ConclusionConclusion

FD-Term Model providesInflationary Mechanism



FD-Term Model providesInflationary MechanismSolution to Gravitino Problem



FD-Term Model providesInflationary MechanismSolution to Gravitino ProblemSolution to µ Problem



FD-Term Model providesInflationary MechanismSolution to Gravitino ProblemSolution to µ ProblemEW Scale Heavy Neutrinos

Seesaw MechanismResonant LeptogenesisLepton Flavor Violating ProcessesAccessible at LHC?



FD-Term Model providesInflationary MechanismSolution to Gravitino ProblemSolution to µ ProblemEW Scale Heavy NeutrinosRight-Handed Sneutrinos as Thermal DM

Low Energy SUSY SpectrumAnnihilation via Higgs Funnel m N LSP

=mH 1/2≈60GeV



FD-Term Model providesInflationary MechanismSolution to Gravitino ProblemSolution to µ ProblemEW Scale Heavy NeutrinosRight-Handed Sneutrinos as Thermal DM

Low Energy SUSY SpectrumAnnihilation via Higgs FunnelInvisible Higgs DecaysSneutrinos within Cascade Decays

m N LSP=mH 1

/2≈60GeV

Education

Sneutrino Cold Dark Matter, Oxford