Future Directions in Parity Violation: From Quarks to the Cosmos

M.J. Ramsey-Musolf

+ many students, post-docs, collaborators, and colleagues

PAVI ‘06

Fundamental Symmetries & Cosmic History

What are the fundamental symmetries that have governed the microphysics of the evolving universe?

• Parity violation as a probe of the proton’sinternal structure (sea quarks, twist)

• Parity violation as probe of the hadronic weak interaction

• Parity violation as a probe of additional symmetries of the early universe

Fundamental Symmetries & Cosmic History

Beyond the SM SM symmetry (broken)

Electroweak symmetry breaking: Higgs ?

Fundamental Symmetries & Cosmic History

Beyond the SM SM symmetry (broken)

Electroweak symmetry breaking: Higgs ?SM “unfinished business”:

What is the internal landscape of the proton?

Sea quarks, gluons, & qq, qqgcorrellations

Preliminary

Probing the strange sea with PV

World Data 4/24/06

GMs = 0.28 +/- 0.20

GEs = -0.006 +/- 0.016

~3% +/- 2.3% of proton magnetic moment

~20% +/- 15% of isoscalar magnetic moment

~0.2 +/- 0.5% of Electric distribution

Courtesy of Kent Pashke (U Mass)

Consistent with s-quark contributions to mP & JP but smaller than early theoretical expectations

Not surprising: ms / ~ 0.15

Challenge for lattice:

Unquenched, light chiral quarks

Probing Higher Twist: Beyond Probing Higher Twist: Beyond the Parton Modelthe Parton Model

Alekhin NNLOMRST NNLOMRST NNLO withBarbieri Target Mass Corrections

• Smooth transition from DIS (solid squares) to resonance region • Resonances oscillate about perturbative curves (quark-hadron duality in transverse channel) - all Q2

•Target mass corrections large and important

2xF2xF1 1 Experimental StatusExperimental Status

Data from JLab E94-110 (nucl-ex/0410027, submitted to PRL) Courtesy C Keppel

~ 50% fluctuations about leading twist

n = 2 Cornwall-Norton Momentsn = 2 Cornwall-Norton Moments

FFLL

2xF2xF11

F2, F1 in excellent agreement with NNLO + TM above Q2 = 2 GeV2

No (or canceling) higher twists

Yet, dominated by large x and resonance region

Remove known HT (a bit novel), the elastic, and there is no more down to Q2 = 0.5 GeV2

The case looks different for FL (data or curve?)

FF22

Where are the qq and qqg correlations ?

Probing Higher Twist with PV

Sacco, R-M preliminary

€

APV Q2

€

y

Looking beyond the parton descriptionPV Deep Ineslastic eD (J Lab 12 GeV)

~0.4%

E=11 GeV =12.50

Different PDF fits

Theoretical Challenges

pQCD evolution of twistfour moments

Lattice QCD for =4 matrix elements

Organizing the program:what kinematics, complementarity with PC F1,2 , …

Fundamental Symmetries & Cosmic History

Beyond the SM SM symmetry (broken)

Electroweak symmetry breaking: Higgs ?

SM “unfinished business”:

How do weak interactions of hadrons reflect the weak qq force ?

Are QCD symmetries (chiral, large NC,…) applicable? Is there a long range weak NN interaction?

Weak Interactions of Hadrons: Strange?

Hyperon weak decays

€

+ → nπ + Σ+ → pπ 0 Σ− → nπ −

Λ → pπ − Λ → nπ 0 Ξ− → Λπ 0 Ξ0 → Λπ 0

€

MB → ′ B π = U B A + Bγ 5[ ]UB

S-Wave: Parity-violating

P-Wave: Parity-conserving

symmetry not sufficient

€

B

€

′ B

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π

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B

€

′ B

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′ ′ B

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π

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B

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′ B

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′ ′ B

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π

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+

€

LWEAKl.o. = d Tr B h+,B[ ]+( ) + f Tr B h+,B[ ]−( )

Weak Interactions of Hadrons: Strange?

€

r + → pγ ,

r Λ → nγ ,K

€

MB → ′ B λ = −i

MB + M ′ B

U σ μν A + Bγ 5( )U F μν

M1 (PC)

€

αB ′ B =2Re A B*

A2

+ B2

€

αB ′ B ~ ms Λχ ~ 0.15

€

α+ p

~ − 0.76 ± 0.08

αΞ 0Σ0 ~ − 0.63± 0.09

Th’y

Exp’t

Breaking of SU(3) sym

E1 (PV)

Are weak interactions of s-quarks a “un-natural” ? Or are their deeper puzzles with the HWI involving all light flavors ?

Weak Interactions of S=0 Hadrons: Strange?

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N

€

Δ

€

γ€

q

€

q

€

W ±,Z 0

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Aγ = 2dΔ

C3V

mN

Λχ

+L

PV Asymmetry

Q2=0: Nonzero

PVES: G0, QWEAK

enhanced dΔ“natural” dΔ

€

Aγ ~ 1×10−6

€

Aγ ~ 5 ×10−8 What does QCD predict ?

ΔS=0 analog of αBB’ : PV E1 N-Δ transition

Zhu, Puglia, Holstein, R-M

Weak Interactions of S=0 Hadrons: Strange?

Use parity-violation to filter out EM & strong interactions

€

N

€

N€

π ±, ρ, ω

Meson-exchange model Seven PV meson-nucleon couplings

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hπ1 , hρ

0,1,2, hω0,1, hρ

1 ′

Desplanques, Donoghue, & Holstein (DDH)

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q

€

q

€

W ±,Z 0

Nuclear effects: W,Z ~ 0.002 fm << Rcore

Is the weak NN force short range ?

T=1 force

T=

0 fo

rce

Long range: π-exchange?

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0+,0

€

0+,1

€

1+,0

€

0+,1

€

β +

€

18F€

18Ne

€

γ Analog 2-body

matrix elements Model independent

hπ ~0

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N

€

N€

π ±, ρ, ω

€

133CsBoulder, atomic PV

Anapole moment

hπ ~ 10 gπ

Is the weak NN force short range ?

€

N

€

N€

π ±, ρ, ω

T=1 force

T=

0 fo

rce

• Problem with expt’s

• Problem with nuc th’y

• Problem with model

• No problem (1)EFT

Hadronic PV: Effective Field Theory

PV Potential

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π

€

+L

€

+L

€

hπNN1

€

s1,2,3, λ t , ρ t

€

π

€

π

€

π

€

π€

+

€

hπNN1

Long Range Short Range Medium Range

O(p-1) O(p) O(p)O(p)

Six constants to O(p)

Zhu, Maekawa, Holstein, R-M, van Kolck ‘05 R-M & Page ‘06

Hadronic PV: Effective Field Theory

PV Current Operators

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hπNN1

€

s1,2,3, λ t , ρ t

€

hπNN1

Long Range Medium Range

O(p-1) O(p) O(p)O(p)

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π

€

π

€

+L

€

π

€

+L

€

C

€

+L

Short Range

€

π

€

π

€

π

€

π€

+

One new O(p) constant

Hadronic PV: Few-Body Systems

€

mN λ pp = −1.22 AL (r p p)

mN ρ t = − 9.35 AL (r n p → dγ)

mN λ pn = 1.6 AL (r p p) − 3.7 AL (

r p α ) + 37 Aγ (

r n p → dγ ) − 2 Pγ (

r n p → dγ)

mN λ t = 0.4 AL (r p p) − 0.7 AL (

r p α ) + 7 Aγ (

r n p → dγ ) + Pγ (

r n p → dγ)

mN λ nn = 1.6 AL (r p p) − 0.7 AL (

r p α ) + 33.3 Aγ (

r n p → dγ ) −1.08 Pγ (

r n p → dγ)+ 0.83

dφnα

dz

†

€

pp = λ s0 + λ s

1 + λ s2 6

λ nn = λ s0 − λ s

1 + λ s2 6

λ pn = λ s0 − 2λ s

2 6

Pionless theory

Done

NIST,SNS

LANSCE, SNS

HARD*

Ab initio few-body calcs

€

AL

r γ d → np( )

€

Aγ

r n d → tγ( )

€

dφnp

dz €

Pγ nd → tγ( )

€

AL

r p d( )

New few-body calcs needed

Pionless th’y: 5 exp’ts Dynamical pions: 7 exp’ts

Hadronic PV: Theoretical Challenges

Attempt to understand the i, hπ etc. from QCD

Attempt to understand nuclear PV observables systematically

Are the PV LEC’s “natural” from QCD standpoint?

Does EFT power counting work in nuclei ?

Complete determination of PV NN & γNN interactions through O (p)

Implications for 0ββ-decay

Hadronic PV & ββ - decay

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e−

€

e−

€

M

€

W −

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W −

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u

€

u

€

d

€

d

€

e−

€

e−

€

0

€

˜ e −

€

u

€

u

€

d

€

d

€

˜ e −

How do we compute & separate heavy particle exchange effects?

Light M : 0ββ-decay rate may yield scale of m

€

mν

EFF= Uek

2mk e2iδ

k

∑

€

e−

€

e−

€

A Z,N( )

€

A Z + 2,N − 2( )

Hadronic PV & ββ - decay

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e−

€

e−

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M

€

W −

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W −

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u

€

u

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d

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d

€

e−

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e−

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0

€

˜ e −

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u

€

u

€

d

€

d

€

˜ e −

€

e−

€

e−

€

A Z,N( )

€

A Z + 2,N − 2( )€

u

€

d€

u

€

d

€

e−

€

e−

4 quark operator, as in hadronic PV

How do we compute & separate heavy particle exchange effects?

Hadronic PV as a probe

€

π

O ( p -1 ) O ( p )

• Determine VPV through O (p) from PV low-energy few-body studies where power counting works

• Re-analyze nuclear PV observables using this VPV

•If successful, we would have some indication that operator power counting works in nuclei

• Apply to ββ-decay

€

N

€

N€

π

€

π€

e−

€

e−

€

N

€

N€

π€

e−

€

e−

€

N

€

N

€

e−

€

e−

€

KNNNN p0

€

KπNN p−1

€

Kππ p−2Prezeau, R-M, & Vogel

Fundamental Symmetries & Cosmic History

Beyond the SM SM symmetry (broken)

Electroweak symmetry breaking: Higgs ?

Puzzles the Standard Model can’t solve

1. Origin of matter2. Unification & gravity

3. Weak scale stability4. Neutrinos

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

PV as a Probe of New Symmetries

Beyond the SM SM symmetry (broken)

Electroweak symmetry breaking: Higgs ?

Puzzles the Standard Model can’t solve

1. Origin of matter2. Unification & gravity

3. Weak scale stability4. Neutrinos

What are the implications of m and PV expts for possible new symmetries & forces?

PV as a Probe of New Symmetries

Beyond the SM SM symmetry (broken)

Electroweak symmetry breaking: Higgs ?

Unseen Forces: Supersymmetry ?

1. Unification & gravity2. Weak scale stability

3. Origin of matter4. Neutrinos

€

μ−

€

μ

€

˜ χ 0

€

˜ μ −

€

˜ ν μ

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e

€

W −

€

e−

PV Correlations in Muon Decay & m

3/4

0

3/4

1

TWIST (TRIUMF)

PV Correlations in Muon Decay & m

Model Independent Analysis

constrained by m

Model Dependent Analysis

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μ−

€

μ

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e

€

W1,2−

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e−

€

MWR (GeV )

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Pμξ

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Pμξδ

ρ€

TWIST ρ

€

TWIST Pμξ

First row CKM

2005 Global fit: Gagliardi et al.

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H 0

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H 0

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H 0

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Z,W

€

€

€

H 0

€

€

Prezeau, Kurylov 05 Erwin, Kile, Peng, R-M 06 m

MPs

Also β-decay, Higgs production

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e−

€

e+€

Constraints on non-SM Higgs production at ILC:

m , μ and βdecay corr

Weak decays & new physics

€

u c t( )

Vud Vus Vub

Vcd Vcs Vcb

Vtd Vts Vtb

⎛

⎝

⎜ ⎜ ⎜

⎞

⎠

⎟ ⎟ ⎟

d

s

b

⎛

⎝

⎜ ⎜ ⎜

⎞

⎠

⎟ ⎟ ⎟

€

n → p e− ν e

A(Z,N) → A(Z −1,N +1) e+ ν e

π + → π 0 e+ ν e

β-decay €

d → u e− ν e

s → u e− ν e

b → u e− ν e

€

GFβ

GFμ

= Vud 1+ Δrβ − Δrμ( )

New physics

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μ−

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μ

€

˜ χ 0

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˜ μ −

€

˜ ν μ

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e

€

W −

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e−

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μ

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μ− €

e

€

e−

€

˜ χ 0

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˜ χ −

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˜ ν μ

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˜ ν e

€

+L

€

+LSUSY€

δOSUSY

OSM~ 0.001

Flavor-blind SUSY-breaking

CKM, (g-2)μ MW, Mt ,…

M˜ μ L >M˜ q LKurylov, R-M

€

+L

€

+LRPV

μ−

ν e e−

νμ

˜ e Rk

12k 12k

e−

d e−

d

˜ q Lj

1j1

1j1

No long-lived LSP or SUSY DM

MW

R Parity Violation

CKM Unitarity

APV

πl2

Kurylov, R-M, Su

CKM unitarity ?

Weak decays & PV

€

n → p e− ν e

A(Z,N) → A(Z −1,N +1) e+ ν e

π + → π 0 e+ ν e

β-decay

€

GFβ

GFμ

= Vud 1+ Δrβ − Δrμ( )

Liquid N2

Be reflector

Solid D2

77 K poly

Tungsten Target

58Ni coated stainless guide

UCN Detector

Flapper valve

LHe

€

dW ∝1 + ar p e ⋅

r p ν

Ee Eν

+ Ar σ n ⋅

r p eEe

+ L

Ultra cold neutrons

LANSCE: UCN “A” NIST, ILL: n Future SNS: n, a,b,A,… Future LANSCE: n

Lifetime & correlations

Weak decays & PV

€

u c t( )

Vud Vus Vub

Vcd Vcs Vcb

Vtd Vts Vtb

⎛

⎝

⎜ ⎜ ⎜

⎞

⎠

⎟ ⎟ ⎟

d

s

b

⎛

⎝

⎜ ⎜ ⎜

⎞

⎠

⎟ ⎟ ⎟

€

d → u e− ν e

s → u e− ν e

b → u e− ν e

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μ−

€

μ

€

˜ χ 0

€

˜ μ −

€

˜ ν μ

€

e

€

W −

€

e−

€

u

€

d€

e

€

e−

€

˜ χ 0

€

˜ χ −€

˜ u

€

˜ ν e

€

+L

€

+LSUSY€

δOSUSY

OSM~ 0.001

Correlations

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dW ∝1 + ar p e ⋅

r p ν

Ee Eν

+ Ar σ n ⋅

r p eEe

+ L

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

β-decay at “RIAcino”?

€

B me Ee( )r σ n ⋅

r p νEν

+ L

Weak decays & PV: Correlations

QuickTime™ and aTIFF (LZW) decompressor

are needed to see this picture.

β-decay correlations

μ-decay -parameter

Fierz int (current)

ΔGF from μ

Profumo, R-M, Tulin

PV w/ radioactive isotopes ?

Probing SUSY with PV eN Interactions

QuickTime™ and aTIFF (Uncompressed) decompressorare needed to see this picture.

SUSY loops

-> eμ+e

SUSY dark matter

Kurylov, Su, MR-M

is Majorana

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

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˜ e −

€

˜ e +

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+L

€

+

€

e−

€

f€

Z 0

€

γ

€

˜ χ −

€

˜ χ +€

e−

€

e−€

e−

€

f

€

f€

f

€

γ

€

Z 0

μ−

ν e e−

νμ

˜ e Rk

12k 12k

Probing SUSY with PV eN Interactions

e

p

RPV

Loops

SUSY effects

Deep Inelastic eD vs elastic ef

Probing SUSY with PV eN Interactions

QuickTime™ and aTIFF (Uncompressed) decompressorare needed to see this picture.

SUSY dark matter

Kurylov, R-M, Su

SUSY loops

RPV 95% CL€

δQWp,SUSY QW

p,SM

€

δQWe,SUSY QW

e,SM

E158 &Q-Weak

JLab Moller

Linear collider

“DIS Parity”

Fundamental Symmetries & Cosmic History

Beyond the SM SM symmetry (broken)

Electroweak symmetry breaking: Higgs ?

Cosmic Energy Budget

?

Baryogenesis: When? SUSY? Neutrinos? CPV?

WIMPy D.M.: Related to baryogenesis?

“New gravity”? Lorentz violation? Effects on CMB?

What is the origin of baryonic matter ?

Cosmic Energy Budget

Baryons

Dark Matter

Dark Energy

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

€

rE

€

rd = d

r S

€

EDM = −d

r S ⋅

r E

h

T-odd , CP-odd by CPT theorem

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

€

YB =ρ B

sγ

=(7.3± 2.5) ×10−11

(9.2 ±1.1) ×10−11

BBN

WMAP

Baryogenesis: New Electroweak Physics

Weak Scale Baryogenesis

• B violation

• C & CP violation

• Nonequilibrium dynamics

Sakharov, 1967

?

ϕ new

?

φ(x)

Unbroken phase

Broken phaseCP Violation

Topological transitions

1st order phase transition

?

γ

?

e -?

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

?

ϕ new

?

ϕ new

90’s: Cohen, Kaplan, Nelson Joyce, Prokopec, Turok

EDM Probes of New CP Violation

f dSM dexp dfuture

€

e−

n199Hg

μ

< 10−40

< 10−30

< 10−33

< 10−28

< 1.6 ×10−27

< 6.3×10−26

< 2.1×10−28

< 1.1×10−18

→ 10−31

→ 10−29

→ 10−32

→ 10−24

CKM

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

Also 225Ra, 129Xe, d

Baryogenesis & Dark Matter: MSSM

Neutralino Mass Matrix

M1

-μ

M2

-mZ cos β sin W mZ cos β cos W

mZ sin β sin W -mZ sin β sin W 0

0

0

0

-μ

-mZ cos β sin W mZ cos β cos W

mZ sin β sin W -mZ sin β sin WMN =

Chargino Mass Matrix

M2

μMC =

βcos2mW

βsin2mWT << TEW : mixing

of H,W to + ~ ~ ~ ~

T ~TEW : scattering

of H,W from

background field

~~

?

ϕ new

?

φ(x)

€

q , ˜ W , ˜ B , ˜ H u,d

T ~ TEW

CPV

B + W + Hd + Hu

BINO WINO HIGGSINO

T << TEW

EDM constraints & SUSY CPV

AMSB: M1 ~ 3M2

Neutralino-driven baryogenesis

Baryogenesis

LEP II Exclusion

Two loop de

Cirigliano, Profumo, R-M

SUGRA: M2 ~ 2M1

Dark Matter: Future Experiments

Cirigliano, Profumo, R-M

EDMs, Baryogenesis, & Dark Matter

• Continued progress in performing systematiccomputations of the baryon asymmetry

• Continued scrutiny of QCD & nuclear structureuncertainties in EDM computations

• Comprehensive phenomenology with othermodels of new CPV (extended Higgssector)

• Funding for experiments !

Future Directions:

• Parity violation in electron scattering and hadronic interactions will continue to provide new insights into proton’s internal structure and weak qq interactions

• PV in weak decays and electron scattering will continue toprovide insights into new physics (SUSY, ’s, Higgs) that will complement LHC, ILC probes

• PVTV will provide powerful probe of the origin of baryonicmatter and non-baryonic dark matter

Considerable theoretical and experimental challenges and opportunities remain: PAVI must go on!