Chiral symmetries and low energy searches for new physics
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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?

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Chiral symmetries and low energy searches for new physics

Chiral Symmetries and Low Energy Searches for New Physics

M.J. Ramsey-Musolf

Caltech

Wisconsin-Madison


Fundamental symmetries cosmic history

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 newsymmetries?


Fundamental symmetries cosmic history1

Electroweak symmetry breaking: Higgs ?

Beyond the SM

SM symmetry (broken)

Fundamental Symmetries & Cosmic History


Fundamental symmetries cosmic history2

Electroweak symmetry breaking: Higgs ?

Beyond the SM

SM symmetry (broken)

Fundamental Symmetries & Cosmic History

Puzzles 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?


What are the new fundamental symmetries

Large Hadron Collider

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 symmetries1

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


Fundamental symmetries cosmic history3

Cosmic Energy Budget

Electroweak symmetry breaking: Higgs ?

Weak scale baryogenesis can be tested experimentally

Beyond the SM

SM symmetry (broken)

Fundamental Symmetries & Cosmic History

Baryogenesis: When? SUSY? Neutrinos? CPV?

WIMPy D.M.: Related to baryogenesis?

“New gravity”? Grav baryogenesis?

?


What is the origin of baryonic matter

Cosmic Energy Budget

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)

What is the origin of baryonic matter ?


Edm probes of new cp violation

CKM

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 Violation


Baryogenesis new electroweak physics

Scale 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?

Baryogenesis: New Electroweak Physics

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

Unbroken phase

CP Violation


Baryogenesis dark matter susy

Supersymmetry

Fermions

Bosons

sfermions

gauginos

Higgsinos

Charginos, neutralinos

Baryogenesis & Dark Matter: SUSY


Baryogenesis dark matter susy1

M1

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: SUSY

Chargino Mass Matrix

Neutralino Mass Matrix


Edm constraints susy cpv

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 CPV


Dark matter future experiments

Assuming Wc ~ WCDM

Cirigliano, Profumo, R-M

Dark Matter: Future Experiments


Precision ewk probes of new symmetries

Electroweak symmetry breaking: Higgs ?

Beyond the SM

SM symmetry (broken)

Precision Ewk Probes of New Symmetries

Unseen Forces: Supersymmetry ?

Unification & gravity

Weak scale stability

Origin of matter

Neutrinos


Weak decays new physics

CKM unitarity ?

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 physics

See Moulson, Cirigliano


Weak decays susy

Correlations

Non (V-A) x (V-A) interactions: me/E

b-decay at SNS,“RIAcino”?

SUSY

Weak decays & SUSY


Weak decays susy correlations

Profumo, R-M, Tulin

Future exp’t ?

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

Yukawa suppressed L-R mixing: “alignment” models

Weak decays & SUSY : Correlations

SUSY loop-induced operators

with mixing between L,R chiral supermultiplets


Pion leptonic decay susy

SM radiative corrections important for precise FpHolstein, Marciano & Sirlin

RPV SUSY

Pion leptonic decay & SUSY

A non-zero DNEW would shift Fp


Pion leptonic decay susy1

Leading QCD uncertainty:

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


Lepton scattering new symmetries

“Weak Charge” ~ 1 - 4 sin2 qW ~ 0.1

Lepton Scattering & New Symmetries

Parity-Violating electron scattering


Probing susy with pv en interactions

n is Majorana

12k

SUSY loops

 SUSY dark matter

12k

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

Probing SUSY with PV eN Interactions

Kurylov, Su, MR-M


Probing susy with pv en interactions1

“DIS Parity”

SUSY loops

E158 &Q-Weak

Linear collider

JLab Moller

RPV 95% CL

Probing SUSY with PV eN Interactions

Kurylov, R-M, Su

 SUSY dark matter

 SUSY dark matter


Fundamental symmetries cosmic history4

Electroweak symmetry breaking: Higgs ?

Beyond the SM

SM symmetry (broken)

Fundamental Symmetries & Cosmic History

Neutrinos ?

LFV & LNV ?

Are they their own antiparticles?

Why are their masses so small?

Can they have magnetic moments?

Implications of mnfor neutrino interactions ?


Neutrino mass magnetic moments

mn< 10-14mB Dirac

mnem< 10-9-10-12mB Majorana

Neutrino Mass & Magnetic Moments

Bell, 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


Muon decay neutrino mass

3/4

0

3/4

1

TWIST (TRIUMF)

Muon Decay & Neutrino Mass


Correlations in muon decay m n

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 & mn

Model Independent Analysis

2005 Global fit: Gagliardi et al.

Model Dependent Analysis


Neutrino mass 0n bb decay

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

How do we compute & separate heavy particle exchange effects?

Neutrino Mass & 0n bb - decay


Neutrino mass 0n bb decay1

How do we compute & separate heavy particle exchange effects?

4 quark operator: low energy EFT

Neutrino Mass & 0n bb - decay


Neutrino mass 0n bb decay2

RPV SUSY

No 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 - decay

Prezeau, R-M, & Vogel


Conclusions

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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