Transcript Document
Future Directions in Parity Violation:
From Quarks to the Cosmos
M.J. Ramsey-Musolf
+ many students, postdocs, collaborators, and
colleagues
PAVI ‘06
MHLOS
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’s
internal 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
Electroweak symmetry
breaking: Higgs ?
Beyond the SM
SM symmetry (broken)
Fundamental Symmetries & Cosmic History
Electroweak symmetry
SMHiggs
“unfinished
business”:
breaking:
?
What is the internal landscape
of the proton?
Sea quarks, gluons, & qq, qqg
correllations
Beyond the SM
SM symmetry (broken)
Probing the strange sea with PV
GMs = 0.28 +/- 0.20
Not surprising:
ms / Lc ~ 0.15
Challenge for
lattice:
Unquenched, light
chiral quarks
Preliminary
World Data
4/24/06
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
Consistent with s-quark
contributions to mP & JP
but smaller than early
theoretical expectations
Courtesy of Kent
Pashke (U Mass)
Probing Higher Twist: Beyond
the Parton Model
2xF1 Experimental Status
Alekhin NNLO
MRST NNLO
MRST NNLO with
Barbieri Target
Mass Corrections
• Smooth transition from DIS
(solid squares) to resonance
region
• Resonances oscillate about
perturbative curves (quarkhadron duality in transverse
channel) - all Q2
•Target mass corrections large
and important
~ 50% fluctuations
about leading twist
Data from JLab E94-110 (nucl-ex/0410027, submitted to PRL) Courtesy C Keppel
n = 2 Cornwall-Norton Moments
F2
2xF1
FL
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 are
looksthe
different
for
Where
qq and
Fqqg
or curve?) ?
L (data
correlations
Probing Higher Twist with PV
Looking
PV
Deepbeyond
Ineslastic
theeD
parton
(J Lab
description
12 GeV)
APV Q 2
Theoretical Challenges
~0.4%
Different
pQCD evolution of twist
PDF fits
four moments
Lattice QCD for t =4
matrix elements
y
Organizing the program:
what kinematics,
complementarity
E=11 GeV
0
with
PC F1,2 , …
q=12.5
Sacco, R-M
preliminary
Fundamental Symmetries & Cosmic History
Electroweak
symmetry business”:
SM “unfinished
breaking: Higgs ?
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?
Beyond the SM
SM symmetry (broken)
Weak Interactions of Hadrons: Strange?
Hyperon weak decays
S n
S p 0
S n
L p
L n 0
L 0 0 L 0
M B B UB A B 5 UB
S-Wave:
Parity-violating
B
Ll.o.WEAK dTrBh,B f TrBh,B
P-Wave:
Parity
conserving
B
c symmetry
not sufficient
B
B
B
B
B
B
Weak Interactions of Hadrons: Strange?
S p , L n ,
E1 (PV)
i
MB B
U A B 5 U F
MB MB
Breaking of
SU(3) sym
M1 (PC)
Are weak interactions of
2Re A B* ?
s-quarks a “un-natural”
Bare
deeper
B their
2
2
Or
A HWI
B
puzzles with the
involving all light flavors ?
BB ~ ms L c ~ 0.15
S
p
~ 0.76 0.08
S ~ 0.63 0.09
0 0
Th’y
Exp’t
Weak Interactions of S=0 Hadrons:
Strange?
Zhu, Puglia, Holstein, R-M
W ,Z 0
q
S=0 analog of BB’ :
PV E1 N- transition
q
N
A ~ 5 108
“natural” d
PV Asymmetry
Q2=0: Nonzero
PVES: G0,
QWEAK
What does
QCD predict ?
d mN
A 2 V
C3 L c
A ~ 1106
enhanced d
Weak Interactions of S=0 Hadrons:
Strange?
W ,Z 0
q
Nuclear effects:
W,Z ~ 0.002 fm << Rcore
q
Meson-exchange model
, ,
N
N
Use parity-violation to filter
out EM & strong interactions
Seven PV mesonnucleon couplings
h1 , h0,1,2 , h0,1, h1
Desplanques, Donoghue,
& Holstein (DDH)
Is the weak NN force short range ?
h ~ 10 g
,
Cs , Anapole
moment
133
Boulder, atomic PV
N
N
h ~0
0
18
Long range:
-exchange?
Ne
,0
0 ,1
T=1 force
0 ,1
1 ,0
18
F
Analog
2-body
matrix elements
Model
independent
Is the weak NN force short range ?
, ,
N
N
• Problem with expt’s
• Problem with nuc th’y
• Problem with model
T=1 force
• No problem (1)
EFT
Hadronic PV: Effective Field Theory
PV Potential
Long Range
Medium Range
Short Range
h1NN
1,2,3
s , t , t
h1NN
O(p)
O(p)
O(p-1)
O(p)
Zhu, Maekawa,
Holstein, R-M, van Kolck ‘05
Six constants to O(p)
R-M & Page ‘06
One new O(p) constant
PV Current Operators
O(p-1)
Long Range
h1NN
Hadronic PV: Effective Field Theory
Medium Range
Short Range
C
h1NN
1,2,3
s , t , t
O(p)
O(p)
O(p)
Hadronic PV: Few-Body Systems
Pionless theory
mN pp 1.22 AL (pp)
Ab initio few-body calcs
Done
LANSCE, SNS
mN t 9.35 AL (np d )
HARD*
mN pn 1.6 AL (pp) 3.7 AL (p ) 37 A (np d ) 2 P (np d )
mN t 0.4 AL (pp) 0.7 AL (p ) 7 A (np d ) P (np d )
d n
mN nn 1.6 AL (pp) 0.7 AL (p ) 33.3 A (np d ) 1.08 P (np d ) 0.83
dz
AL d np P nd t
0
1
2
6
pp s s s
NIST,SNS
A nd t AL pd
nn 0s 1s 2s
6
d np
New 2few-body
Pionless th’y: 5 exp’ts
0
s calcs
2 sneeded
6
dzpn
Dynamical pions: 7 exp’ts
Hadronic PV: Theoretical Challenges
Complete determination of PV NN &
NN interactions through O (p)
Attempt to understand
the i, h 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 ?
Implications for 0-decay
Hadronic PV & 0 - decay
e
e
e
AZ,N
u
AZ 2,N 2
How do we compute & separate
exchange effects?
heavy particle
e
M
W
W
d
u
d
e
e
Light M : 0-decay
rate may
0 scale of
yield
c
m e˜
u
e˜
u
EFF
2
m
U ek mk e 2i
d k
d
Hadronic PV & 0 - decay
How do we compute & separate
heavy particle exchange effects?
e e
u
d
AZ,N
e
e e
u
u
AZ 2,Nd 2
e
u
W
4 quark operator,
as in hadronic PV
M
W
d
e
e˜
d
e
c 0
e˜
d
u
d
u
Hadronic PV as a probe
• Determine VPV through O (p)
from PV low-energy few-body
studies where power counting
works
O ( p -1 )
e
• Re-analyze nuclear PV
observables using this VPV
O ( p)
e
e
e
e
e we would have some
•If successful,
indication
that operator
power
counting works in nuclei
N
N
•
Apply
to
0-decay
N
K p2
N
K NN p1
N
N
K NNNN p 0
Prezeau, R-M,
& Vogel
Fundamental Symmetries & Cosmic History
Electroweak
symmetry
Puzzles the Standard
Model
can’t solve
breaking: Higgs ?
1.
2.
3.
4.
Origin of matter
Unification & gravity
Weak scale stability
Neutrinos
Beyond the SM
What are the symmetries
(forces) of the early
universe beyond those of
the SM?
SM symmetry (broken)
PV as a Probe of New Symmetries
Electroweak
symmetry
Puzzles the Standard
Model
can’t solve
breaking: Higgs ?
1.
2.
3.
4.
Origin of matter
Unification & gravity
Weak scale stability
Neutrinos
Beyond the SM
What are the implications
of m and PV expts for
possible new symmetries
& forces?
SM symmetry (broken)
PV as a Probe of New Symmetries
Electroweak
symmetry?
Unseen Forces:
Supersymmetry
breaking: Higgs ?
1.
2.
3.
4.
Unification & gravity
Weak scale stability
Origin of matter
Neutrinos
˜
e
W
˜0
c
˜
e
Beyond the SM
SM symmetry (broken)
PV Correlations in Muon Decay & m
3/4
0
3/4
1
TWIST (TRIUMF)
PV Correlations in Muon Decay & m
Model Independent
Analysis
0
0
H
H
H
0
e
MPs
constrained by m
1,2
m , and decay corr
P
e
TWIST P
W
Also -decay,
Higgs production
e
e
m
Erwin, Kile, Peng, R-M 06
Constraints on non-SM
Higgs production at ILC:
Model Dependent Analysis
H0
Z,W
Prezeau,Kurylov 05
2005 Global fit: Gagliardi et al.
TWIST
First row CKM
P
MWR (GeV)
Weak decays & new physics
R Parity Violation
R-M,
V Flavor-blind
dSu
VKurylov,
VSUSY-
d u e e
ud
us
breaking
u c t Vcd
V
MW td
s u e e
b u e e
e
e
O
c
~ 0.001
SM
12k
12k ˜
n p e e e O
-decay
e˜
˜
˜
0
e
SUSY
k
W
R
d
ee
˜e
e e
˜
c
e
0
j
L
˜
1j1
A(Z,N)q˜ A(Z 1,N 1) e e
˜0
c
1j1
e d
CKM unitarity ?
ub
Vcs Vcb s
CKM Unitarity
Vts Vtb b
CKM, (g-2),
MW, Mt ,…
F
F
APV
l2
G
Vud 1 r r
G
M˜ L Mq˜ L
Kurylov,
No
long-lived LSPNew
or SUSY
physics
DMR-M
SUSY
RPV
Weak decays & PV
F
F
G
Vud 1 r r
G
Ultra cold neutrons
58Ni
coated stainless guide
-decay
n p e e
A(Z,N) A(Z 1,N 1) e e
0 e e
Lifetime & correlations
Flapper valve
Liquid N2
pe p
pe
dW 1 a
An
E e E
Ee
Be reflector
LHe
Solid D2
77 K poly
UCN Detector
Tungsten Target
LANSCE: UCN “A”
NIST, ILL:
tn
Future SNS: tn,
a,b,A,… Future LANSCE:
Correlations
Weak decays & PV
d u e e
u
s u e e
b u e e
˜
W
˜0
c
e
u˜
d
Vus Vub d
Vcs Vcb s
Vts Vtb b
pe p
ppe
dW 1 a Bme Ee An n
E e E
EE e
˜0
c
u
˜
O
~ 0.001
SM
O
e
SUSY
c
Vud
t Vcd
Vtd
e
˜e
˜
c
e
SUSY
Non (V-A) x (V-A)
interactions: me/E
-decay at “RIAcino”?
Weak decays & PV: Correlations
Fierz int
(current)
-decay
correlations
QuickTime™ and a
TIFF (LZW) decompressor
are needed to see this picture.
-decay hparameter
Profumo, R-M, Tulin
PV w/
radioactive
isotopes ?
GF from
t
Probing SUSY with PV eN Interactions
e
Z
SUSY
dark matter
e
0
˜
c
Z0
f
c
SUSY
loops
˜
e˜
e
f
e
e˜
f
f
c0 ->
QuickTime™ and a TIFF (Uncompressed)
e+e decompressor are needed to see this picture.
is Majorana
e
e
˜ Rk
e
RPV 95% CL fit to
12k decays, M ,etc.
12k
weak
W
Kurylov, Su, MR-M
Probing SUSY with PV eN Interactions
Deep Inelastic eD vs elastic ef
e
RPV
Loops
p
SUSY effects
Probing SUSY with PV eN Interactions
Kurylov, R-M, Su
“DIS Parity”
SUSY loops
SUSY
dark matter
QWp,SUSYQuickTime™
QWp,SM and a TIFF (Uncompressed) decompressor are needed to see this picture.
Linear
collider
E158 &QWeak
JLab Moller
RPV 95% CL
QWe, SUSY QWe, SM
Fundamental Symmetries & Cosmic History
Electroweak symmetry
breaking: Higgs ?
Baryogenesis: When?
SUSY? Neutrinos? CPV?
WIMPy D.M.: Related
to baryogenesis?
“New gravity”? Lorentz
violation? Effects on CMB?
?
Beyond the SM
SM symmetry (broken)
Cosmic Energy Budget
What is the origin of baryonic matter ?
Cosmic Energy Budget
E
d dS
Dark Matter
Baryons
EDM
B (7.3 2.5) 1011
YB
s (9.2 1.1) 1011
BBN
WMAP
Dark Energy
dS E
h
T-odd , CP-odd
by CPT theorem
What are the
Searches
for permanent
quantitativeelectric
implications
dipoleof new
moments
EDM
experiments
(EDMs) of
forthe
explaining
neutron,the
electron,
origin of
andbaryonic
the
neutral atoms
component
probe of
new
theCP-violation
Universe ?
Baryogenesis: New Electroweak Physics
90’s:
Weak Scale Baryogenesis
• B violation
Cohen, Kaplan, Nelson
Joyce, Prokopec, Turok
Unbroken phase
Topological transitions
new
• C & CP violation
• Nonequilibrium
dynamics
(x)
Broken phase
1st order phase transition
CP Violation
Sakharov, 1967
new
• Is it viable?
• Can experiment constrain it?
• How reliably can we compute it?
new
new
e
EDM Probes of New CP Violation
CKM
f
dSM
dexp
dfuture
e
1040
1.6 1027
1031
n
1030
6.3 1026
1029
Hg
1033
2.11028
1032
1028
1.11018
1024
199
Also 225Ra, 129Xe, d
If new EWK CP violation is responsible for abundance
of matter, will these experiments see an EDM?
Baryogenesis & Dark Matter: MSSM
Chargino Mass Matrix
T << TEW
CPV
new
0
0
0
0
M
c
C =11B 12W 13Hd 14Hu
mW 2 sin
WINO
M1
0
HIGGSINO
Neutralino Mass Matrix
MN =
background field
m W 2 cos
M2
BINO
T ~TEWT:~scattering
TEW
~ ~
(xH,W
)
of
from
T << TEW : mixing
~ ~
~0
of H,W to c~,c
q , W˜ , B˜ , H˜ u,d
0
-mZ cos sin qW
mZ cos cos qW
M2
mZ sin sin qW
-mZ sin sin qW
-mZ cos sin qW
mZ cos cos qW
0
-
mZ sin sin qW
-mZ sin sin qW
-
0
EDM constraints & SUSY CPV
Neutralino-driven
baryogenesis
Baryogenesis
LEP II Exclusion
Two loop de
Cirigliano,
Profumo, R-M
SUGRA: M2 ~ 2M1
AMSB: M1 ~ 3M2
Dark Matter: Future Experiments
Cirigliano,
Profumo, R-M
EDMs, Baryogenesis, & Dark Matter
• Continued progress in performing systematic
computations of the baryon asymmetry
• Continued scrutiny of QCD & nuclear structure
uncertainties in EDM computations
• Comprehensive phenomenology with other
models of new CPV (extended Higgs
sector)
• 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 to
provide insights into new physics (SUSY, ’s, Higgs)
that will complement LHC, ILC probes
• PVTV will provide powerful probe of the origin of baryonic
matter and non-baryonic dark matter
Considerable theoretical and experimental challenges
and opportunities remain: PAVI must go on!