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Chiral Symmetries and Low Energy Searches for New PhysicsPowerPoint Presentation

Chiral Symmetries and Low Energy Searches for New Physics

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### What is the origin of baryonic matter ?

Chiral Symmetries and Low Energy Searches for New Physics

M.J. Ramsey-Musolf

Caltech

Wisconsin-Madison

Fundamental Symmetries & Cosmic History

- What were the fundamental symmetries that governed the microphysics of the early universe?
- Were there additional (broken) chiral symmetries?
- What insights can low energy (E << MZ) precision electroweak studies provide?
- How does the approximate chiral symmetry of QCD the affect low energy search for new symmetries?

Electroweak symmetry breaking: Higgs ?

Beyond the SM

SM symmetry (broken)

Fundamental Symmetries & Cosmic HistoryElectroweak symmetry breaking: Higgs ?

Beyond the SM

SM symmetry (broken)

Fundamental Symmetries & Cosmic HistoryPuzzles the Standard Model can’t solve

Origin of matter

Unification & gravity

Weak scale stability

Neutrinos

What are the symmetries (forces) of the early universe beyond those of the SM?

Ultra cold neutrons

LANSCE, NIST, SNS, ILL

CERN

What are the new fundamental symmetries?Two frontiers in the search

Collider experiments (pp, e+e-, etc) at higher energies (E >> MZ)

Indirect searches at lower energies (E < MZ) but high precision

Particle, nuclear & atomic physics

High energy physics

What are the new fundamental symmetries?

- Why is there more matter than antimatter in the present universe?
- What are the unseen forces that disappeared from view as the universe cooled?
- What are the masses of neutrinos and how have they shaped the evolution of the universe?

Electric dipole moment & dark matter searches

Precision electroweak: weak decays & e- scattering

Neutrino interactions & 0nbb-decay

Tribble report

Electroweak symmetry breaking: Higgs ?

Weak scale baryogenesis can be tested experimentally

Beyond the SM

SM symmetry (broken)

Fundamental Symmetries & Cosmic HistoryBaryogenesis: When? SUSY? Neutrinos? CPV?

WIMPy D.M.: Related to baryogenesis?

“New gravity”? Grav baryogenesis?

?

Dark Matter

BBN

WMAP

Searches for permanent electric dipole moments (EDMs) of the neutron, electron, and neutral atoms probe new CP-violation

Dark Energy

T-odd , CP-odd by CPT theorem

Baryons

What are the quantitative implications of new EDM experiments for explaining the origin of the baryonic component of the Universe ?

Chiral odd

SU(2)L x U(1)Y invariant for L >> Mweak

SM CPV Yukawa suppressed

Beyond SM CPV may not be (e.g., SUSY)

fdSM dexp dfuture

Also 225Ra, 129Xe, d

If new EWK CP violation is responsible for abundance of matter, will these experiments see an EDM?

EDM Probes of New CP ViolationScale Hierarchy: Expand in energy & time scale ratios

Weak Scale Baryogenesis

Cirigliano, Lee, R-M

- B violation
- C & CP violation
- Nonequilibrium dynamics

Topological transitions

Theoretical Issues:

Transport at phase boundary (non-eq QFT)

Bubble dynamics (numerical)

Strength of phase transition (Higgs sector)

EDMs: many-body physics & QCD

Broken phase

1st order phase transition

Sakharov, 1967

- Is it viable?
- Can experiment constrain it?
- How reliably can we compute it?

90’s: Cohen, Kaplan, NelsonJoyce, Prokopec, Turok

Unbroken phase

CP Violation

Fermions

Bosons

sfermions

gauginos

Higgsinos

Charginos, neutralinos

Baryogenesis & Dark Matter: SUSYM1

0

-mZ cosb sinqW

mZ cosb cosqW

T ~TEW : scattering of H,W from background field

MN =

~

~

T ~ TEW

mZ sinb sinqW

M2

-mZ sinb sinqW

0

CPV

0

-m

-mZ cosb sinqW

mZ cosb cosqW

-m

T << TEW : mixing of H,W to c+, c0

mZ sinb sinqW

-mZ sinb sinqW

0

~

~

~

~

M2

- = N11B 0 + N12W 0 + N13Hd0 + N14Hu0

MC =

m

T << TEW

BINO

WINO

HIGGSINO

Baryogenesis & Dark Matter: SUSYChargino Mass Matrix

Neutralino Mass Matrix

Neutralino-driven baryogenesis

Baryogenesis

| sin fm | > 0.02

| de , dn | > 10-28 e-cm

Mc < 1 TeV

LEP II Exclusion

Two loop de

Cirigliano, Profumo, R-M

SUGRA: M2 ~ 2M1

AMSB: M1 ~ 3M2

EDM constraints & SUSY CPVElectroweak symmetry breaking: Higgs ?

Beyond the SM

SM symmetry (broken)

Precision Ewk Probes of New SymmetriesUnseen Forces: Supersymmetry ?

Unification & gravity

Weak scale stability

Origin of matter

Neutrinos

Flavor-blind SUSY-breaking

12k

R ParityViolation

Kurylov, R-M, Su

CKM Unitarity

MW

CKM, (g-2)m, MW, Mt ,…

APV

l2

b-decay

12k

1j1

1j1

No long-lived LSP or SUSY DM

New physics

Kurylov, R-M

RPV

SUSY

Weak decays & new physicsSee Moulson, Cirigliano

Future exp’t ?

Large L-R mixing: New models for SUSY-breaking

Yukawa suppressed L-R mixing: “alignment” models

Weak decays & SUSY : CorrelationsSUSY loop-induced operators

with mixing between L,R chiral supermultiplets

SM radiative corrections important for precise FpHolstein, Marciano & Sirlin

RPV SUSY

Pion leptonic decay & SUSYA non-zero DNEW would shift Fp

Marciano & Sirlin

Probing Slepton Universality

vs

Min

(GeV)

Tulin, Su, R-M Prelim

New TRIUMF, PSI

Can we do better on

?

Pion leptonic decay & SUSY“Weak Charge” ~ 1 - 4 sin2 qW ~ 0.1

Lepton Scattering & New SymmetriesParity-Violating electron scattering

n is Majorana

12k

SUSY loops

SUSY dark matter

12k

RPV 95% CL fit to weak decays, MW, etc.

Probing SUSY with PV eN InteractionsKurylov, Su, MR-M

SUSY loops

E158 &Q-Weak

Linear collider

JLab Moller

RPV 95% CL

Probing SUSY with PV eN InteractionsKurylov, R-M, Su

SUSY dark matter

SUSY dark matter

Electroweak symmetry breaking: Higgs ?

Beyond the SM

SM symmetry (broken)

Fundamental Symmetries & Cosmic HistoryNeutrinos ?

LFV & LNV ?

Are they their own antiparticles?

Why are their masses so small?

Can they have magnetic moments?

Implications of mnfor neutrino interactions ?

mn< 10-14mB Dirac

mnem< 10-9-10-12mB Majorana

Neutrino Mass & Magnetic MomentsBell, Cirigliano, Gorshteyn,R-M, Vogel, Wang, Wise Davidson, Gorbahn, Santamaria

How large is mn ?

Experiment: mn< (10-10 - 10-12) mB

e scattering, astro limits

Radiatively-induced mn

Both operators chiral odd

mn

MPs

Constraints on non-SM Higgs production at ILC:

mn , m- and b-decay corr

constrained by mn

Also b-decay, Higgs production

Erwin, Kile, Peng, R-M 06

Prezeau, Kurylov 05

First row CKM

Correlations in Muon Decay & mnModel Independent Analysis

2005 Global fit: Gagliardi et al.

Model Dependent Analysis

Light nM : 0nbb-decay rate may yield scale of mn

How do we compute & separate heavy particle exchange effects?

Neutrino Mass & 0n bb - decayHow do we compute & separate heavy particle exchange effects?

4 quark operator: low energy EFT

Neutrino Mass & 0n bb - decayNo WR - WL mixing

WR - WL mix

L(q,e) =

Chiral properties of Oj++ determine p-dependence of Kpp , KpNN , KNNNN

Kpp ~ O (p0)

Kpp ~ O (p2)

Neutrino Mass & 0n bb - decayPrezeau, R-M, & Vogel

Conclusions

- Low energy probes of physics beyond the SM give us a unique window on the fundamental symmetries of the early universe that complements direct searches for new physics at colliders
- These symmetries - including broken chiral symmetries - are needed to explain the origin of matter, provide for stability of the electroweak scale, incorporate new forces implied by unification, and account for the properties of neutrinos
- The broken chiral symmetry of QCD also provides an important tool for sharpening Standard Model predictions for low energy observables and making any deviations interpretable in terms of new symmetries

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