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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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Chiral Symmetries and Low Energy Searches for New Physics

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Chiral Symmetries and Low Energy Searches for New Physics

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M.J. Ramsey-Musolf

Caltech

Wisconsin-Madison

- 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?

Electroweak symmetry breaking: Higgs ?

Beyond the SM

SM symmetry (broken)

Electroweak symmetry breaking: Higgs ?

Beyond the SM

SM symmetry (broken)

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?

Large Hadron Collider

Ultra cold neutrons

LANSCE, NIST, SNS, ILL

CERN

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

- 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

Cosmic Energy Budget

Electroweak symmetry breaking: Higgs ?

Weak scale baryogenesis can be tested experimentally

Beyond the SM

SM symmetry (broken)

Baryogenesis: When? SUSY? Neutrinos? CPV?

WIMPy D.M.: Related to baryogenesis?

“New gravity”? Grav baryogenesis?

?

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 ?

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?

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?

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

Unbroken phase

CP Violation

Supersymmetry

Fermions

Bosons

sfermions

gauginos

Higgsinos

Charginos, neutralinos

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

Chargino 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

Assuming Wc ~ WCDM

Cirigliano, Profumo, R-M

Electroweak symmetry breaking: Higgs ?

Beyond the SM

SM symmetry (broken)

Unseen Forces: Supersymmetry ?

Unification & gravity

Weak scale stability

Origin of matter

Neutrinos

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

See Moulson, Cirigliano

Correlations

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

b-decay at SNS,“RIAcino”?

SUSY

Profumo, R-M, Tulin

Future exp’t ?

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

Yukawa suppressed L-R mixing: “alignment” models

SUSY loop-induced operators

with mixing between L,R chiral supermultiplets

SM radiative corrections important for precise FpHolstein, Marciano & Sirlin

RPV SUSY

A non-zero DNEW would shift Fp

Leading QCD uncertainty:

Marciano & Sirlin

Probing Slepton Universality

vs

Min

(GeV)

Tulin, Su, R-M Prelim

New TRIUMF, PSI

Can we do better on

?

“Weak Charge” ~ 1 - 4 sin2 qW ~ 0.1

Parity-Violating electron scattering

n is Majorana

12k

SUSY loops

SUSY dark matter

12k

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

Kurylov, Su, MR-M

“DIS Parity”

SUSY loops

E158 &Q-Weak

Linear collider

JLab Moller

RPV 95% CL

Kurylov, R-M, Su

SUSY dark matter

SUSY dark matter

Electroweak symmetry breaking: Higgs ?

Beyond the SM

SM symmetry (broken)

Neutrinos ?

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

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

3/4

0

3/4

1

TWIST (TRIUMF)

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

Model 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?

How do we compute & separate heavy particle exchange effects?

4 quark operator: low energy EFT

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)

Prezeau, R-M, & Vogel

- 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