nuclear physics and the new standard model m.j. ramsey-musolf wisconsin-madison npac theoretical...
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Nuclear Physics and the New Standard ModelM.J. Ramsey-MusolfWisconsin-MadisonQuickTime™ and aTIFF (Uncompressed) decompressorare needed to see this picture.
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http://www.physics.wisc.edu/groups/particle-theory/
NPACTheoretical Nuclear, Particle, Astrophysics & Cosmology
Taiwan , June 2008
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The Big Picture
Fifty years of PV in nuclear physics
Nuclear physics studies of s & fundamental symmetries played an essential role in developing & confirming the Standard Model
Our role has been broadly recognized within and beyond NP
Solar s & the neutrino revolution
The next decade presents NP with a historic opportunity to build on this legacy in developing the “new Standard Model”
The value of our contribution will be broadly recognized outside the field
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Goals
• Show how studies of fundamental symmetries & neutrinos in nuclear physics can complement high energy searches for the “new Standard Model”
• Introduce some of the basic ideas & theoretical machinery, but leave details to your future reading
• Describe recent progress & open problems
• Encourage you to learn more and get involved in research !
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Outline
I. Overview & Motivation
II. Illustrative Scenario: Supersymmetry
III. Neutrinos: Lepton Number &
IV. EDMs & the Origin of Matter
V. Electroweak Precision Observables
VI. Weak Decays
VII. Neutral Current Processes
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References
• “ Low Energy Precision Test of Supersymmetry”, M.J. Ramsey-Musolf & S. Su, Phys.Rept.456:188, 2008, e-
Print: hep-ph/0612057Model”
• “Low energy tests of the weak interaction”, J. Erler & M. J. Ramsey-Musolf , Prog.Part.Nucl.Phys.54:351 442, 2005, e-Print: hep-ph/0404291
Plus many references therein…
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• Why New Symmetries ?
• Why Low Energy Probes ?
I. Motivation
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Fundamental Symmetries & Cosmic History
Beyond the SM SM symmetry (broken)
Electroweak symmetry breaking: Higgs ?
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Fundamental Symmetries & Cosmic History
Standard Model puzzles Standard Model successes
to explain the microphysics of the present universe
It utilizes a simple and elegant symmetry principle
SU(3)c x SU(2)L x U(1)Y
• Big Bang Nucleosynthesis (BBN) & light element abundances
• Weak interactions in stars & solar burning
• Supernovae & neutron stars
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Fundamental Symmetries & Cosmic History
Standard Model puzzles Standard Model successesHow is electroweak symmetry broken? How do elementary particles get mass ?
Puzzles the St’d Model may or may not solve:
SU(3)c x SU(2)L x U(1)Y
Electroweak symmetry breaking: Higgs ?
U(1)EM
• Non-zero vacuum expectation value of neutral Higgs breaks electroweak sym and gives mass:
• Where is the Higgs particle?
• Is there more than one?
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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?
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Fundamental Symmetries & Cosmic History
Beyond the SM SM symmetry (broken)
Electroweak symmetry breaking: Higgs ?
Cosmic Energy Budget
?
Baryogenesis: When? CPV? SUSY? Neutrinos?
WIMPy D.M.: Related to baryogenesis?
“New gravity”? Lorentz violation? Grav baryogen ?
• C: Charge Conjugation
• P: Parity
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4πgi
2
log10(μ / μ0)
Standard Model
Present universe Early universe
Weak scale Planck scale
High energy desert
Fundamental Symmetries & Cosmic History
Unification?
Use gauge coupling energy-dependence look back in time
Energy Scale ~ T
€
e = e(μ)
g = g(μ)
€
+L
€
+
€
+
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4πgi
2
log10(μ / μ0)
Standard Model
Present universe Early universe
Weak scale Planck scale
High energy desert
Gravity
Fundamental Symmetries & Cosmic History
4πgi
2A “near miss” for grand unification
Is there unification? What new forces are responsible ?
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log10(μ / μ0)
Standard Model
Present universe Early universe
Planck scale
High energy desert
Weak scale
4πgi
2Weak scale unstable:
Why is GF
so large?
UnificationNeutrino mass Origin of matter
Fundamental Symmetries & Cosmic History
Weak Int Rates:Solar burningElement abundances
€
GF ~ 1 MWEAK2
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There must have been additional symmetries in the earlier Universe to
• Unify all matter, space, & time
• Stabilize the weak scale
• Produce all the matter that exists
• Account for neutrino properties
• Give self-consistent quantum gravity
Supersymmetry, GUT’s, extra dimensions…
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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
High energy physics
Particle, nuclear & atomic physics
CERN
Ultra cold neutronsLarge Hadron Collider
LANSCE, NIST, SNS, ILL
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Precision Probes of New Symmetries
Beyond the SM SM symmetry (broken)
Electroweak symmetry breaking: Higgs ?
New Symmetries
1. Origin of Matter2. Unification & gravity
3. Weak scale stability4. Neutrinos
€
μ−
€
μ
€
˜ χ 0
€
˜ μ −
€
˜ ν μ
€
e
€
W −
€
e−
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?
LHC: energy frontier
Low-energy: precision frontier
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Precision & Energy Frontiers
Radiative corrections
Direct Measurements
Stunning SM Success
J. Ellison, UCI
€
GFZ
GFμ
≈ 1+ ΔrZ − Δrμ( )
€
t
€
t
€
Z 0
€
Z 0
€
t
€
b
€
W +
€
W +
• Precision measurements predicted a range for mt
before top quark discovery
• mt >> mb !
• mt is consistent with that range
• It didn’t have to be that way
Probing Fundamental Symmetries beyond the SM:
Use precision low-energy measurements to probe virtual effects of new symmetries & compare with collider results
Precision Frontier:
• Precision ~ Mass scale
• Look for pattern from a variety of measurements
• Identify complementarity with collider searches
• Special role: SM suppressed processes
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Precision, low energy measurements can probe for new symmetries in the desert
Precision ~ Mass Scale
€
δNEW =ΔONEW
OSM≈
α
π
M˜ M
⎛
⎝ ⎜
⎞
⎠ ⎟2 M=mμ δ ~ 2 x 10-9
δexp ~ 1 x 10-9
M=MW δ ~ 10-3
Interpretability
• Precise, reliable SM predictions
• Comparison of a variety of observables
• Special cases: SM-forbidden or suppressed processes
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• Why Supersymmetry ?
• Key Features of SUSY
II. Illustrative Case: SUSY
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4πgi
2
log10(μ / μ0)
Standard Model
Present universe Early universe
Weak scale Planck scale
Couplings unify with SUSY
Supersymmetry
High energy desert
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GF is Too Large
€
GF
2=
g2
8MW2
=1
2 μWEAK2
GF ~ 10-5/MP2 μWEAK ~ 250 GeV
€
H 0
€
H 0
€
ϕ NEW
€
ΔμWEAK2 ~ Mϕ
2
€
mh2 = 2λ μWEAK
2
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SUSY protects GF
€
H 0
€
H 0
€
˜ ϕ NEW
€
ΔμWEAK2 ~ Mϕ
2 − M ˜ ϕ 2 + log terms
=0 if SUSY is exact
€
H 0
€
H 0
€
ϕ NEW
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GF & the “hierarchy problem”
SUSY Relation:
Quadratic divergence ~ UV2 cancels
After EWSB:
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SUSY may help explain observed abundance of matter
Cold Dark Matter Candidate
0 Lightest SUSY particle
Baryonic matter: electroweak phase transition
˜ t HUnbroken phase
Broken phase
CP Violation
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SUSY: a candidate symmetry of the early Universe
• Unify all forces
• Protect GF from shrinking
• Produce all the matter that exists
• Account for neutrino properties
• Give self-consistent quantum gravity
3 of 4
Yes
Maybe so
Maybe
Probably necessary
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Minimal Supersymmetric Standard Model (MSSM)
Supersymmetry
eL,R , qL,R
W,Z,γ,g
˜ W , ˜ Z ,˜ γ , ˜ H u,d ⇒ ˜ χ ±, ˜ χ 0Charginos, neutralinos
Fermions Bosons
˜ e L,R , ˜ q L,R sfermions
˜ W , ˜ Z ,˜ γ , ˜ g gauginos
˜ H u,˜ H dHiggsinos
€
Hu,Hd
No new coupling constants
Two Higgs vevs
Supersymmetric Higgs mass, μ
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SUSY and R Parity PR = −1( )3(B−L)
−1( )2S
If nature conserves PR vertices have even number of superpartners
Consequences
Lightest SUSY particle˜ χ 0( ) is stable
viable dark matter candidate
Proton is stable
Superpartners appear only in loops
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WRPV = ijk LiLjEk + ijk LiQjDk +μ/
i LiHu
+ ijkUiDjDk
ΔL=1
ΔB=1
Li, Qi
Ei, Ui, Di
SU(2)L doublets
SU(2)L singlets
proton decay: Set
ijk =0
R-Parity Violation (RPV)“Superpotential” : a convenient way to derive supersymmetric interactions by taking derivatives w.r.t. scalar fields
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Four-fermion Operators
μ−
ν e e−
νμ
˜ e Rk
12k 12k
e−
d e−
d
˜ q Lj
1j1
1j1
ΔL=1 ΔL=1
Δ12k =λ12k
2
4 2GF M˜ e Rk
2 Δ1j1/ =
λiji/ 2
4 2GFM˜ q Lj
2
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SUSY must be a broken symmetry
Visible World
Hidden World
Flavor-blind mediation
SUSY Breaking
€
M ˜ e >> me
M ˜ q >> mq
M ˜ χ >> MW ,Z ,γ
Superpartners have not been seen
Theoretical models of SUSY breaking
How is SUSY broken?
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MSSM SUSY Breaking
Superpartners have not been seen
Theoretical models of SUSY breaking
How is SUSY broken?
~ 100 new parameters40 new CPV phasesFlavor mixing parameters
Gaugino mass
Sfermion mass
Triscalar interactions
O(1) CPV phases & flavor mixing ruled out by expt: “SUSY CP” & “SUSY flavor” problems
One solution: af ~ Yf
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MSSM: SUSY Breaking Models I
Flavor-blind mediation
Visible Sector: Hidden Sector: SUSY-breakingMSSM
Gravity-Mediated (mSUGRA)
M1/2 M02 A0 b0
˜ W , ˜ Z ,˜ γ , ˜ g ˜ f
˜ f ˜ f
HHu Hd
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MSSM: SUSY Breaking Models II
Flavor-blind mediation
Visible Sector: Hidden Sector: SUSY-breakingMSSM
Gauge-Mediated (GMSB)
˜ W , ˜ Z ,˜ γ , ˜ g
M1/2 ≈αa
4πΛ M0
2 ≈Λ2 αa
4π⎛ ⎝
⎞ ⎠ Ca∑
˜ f W,Z,...
A0 ≈0b0 ≈0
messengers
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MSSM: SUSY Breaking Models III
Flavor-blind mediation
Visible Sector: Hidden Sector: SUSY-breakingMSSM
dM˜ f
2
dt=− αaCa
˜ f
a=1
3
∑ ˜ M a2
Parameter evolution: mass
M˜ q >M˜ l
at the weak scale
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Gaugino-Higgsino Mixing
Neutralino Mass Matrix
M1
-μ
M2
-mZ cos sin W mZ cos cos W
mZ sin sin W -mZ sin sin W 0
0
0
0
-μ
-mZ cos sin W mZ cos cos W
mZ sin sin W -mZ sin sin WMN =
Chargino Mass Matrix
M2
μMC =
cos2mW
sin2mWT << TEW : mixing
of H,W to ~ ~ ~ ~
T ~TEW : scattering
of H,W from
background field
~~CPV
B W Hd Hu
BINO WINO HIGGSINO
T << TEW
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Relic Abundance of SUSY DM
Neutralino Mass Matrix
M1
-μ
M2
-mZ cos sin W mZ cos cos W
mZ sin sin W -mZ sin sin W 0
0
0
0
-μ
-mZ cos sin W mZ cos cos W
mZ sin sin W -mZ sin sin WMN =
T << TEW : mixing
of H,W to ~ ~ ~ ~
B W Hd Hu
BINO WINO HIGGSINO
€
˜ χ 10
€
˜ χ 10
€
˜ t
€
t
€
t
+ res0
1~
01
~±ji χχ ~,~0
ZW ,
ZW ,+ coannihilation
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Sfermion Mixing
Sfermion mass matrix
€
ˆ M 2 =˜ M ̃ f L
2 MLR2
MLR2 ˜ M ̃ f R
2
⎡
⎣ ⎢ ⎢
⎤
⎦ ⎥ ⎥
MLR2 =
mf (μtanβ −Af )
mf (μcotβ −Af )⎧ ⎨ ⎩
Qf < 0
Qf > 0
T << TEW : mixing
of fL, fR to f1, f2
~ ~ ~ ~
T ~TEW : scattering
of fL, fR from
background field
~~
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Test
€
H 0
€
H 0
€
˜ ϕ NEW
€
H 0
€
H 0
€
ϕ NEW
No new coupling constants
Two Higgs vevs
Supersymmetric Higgs mass, μ
~ 100 new parameters40 new CPV phasesFlavor mixing parameters
“Superpotential” : a convenient way to derive supersymmetric interactions by taking derivatives w.r.t. scalar fields
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Neutral Current Interactions II
Neutral current l+f --> l+f at one loop:
Normalization:
Vector & axial vector couplings:
Normalize to Gμ: Remove Δrμ
Weak mixing:
Vertex & ext leg
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The parameter:
Weak mixing:
Can impose constraints from global fits to EWPO via S,T,U-dependence of these quantities