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Nuclear Physics and the New Standard Model

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... nuclear physics can complement high energy searches for the 'new Standard Model' ... mt is consistent with that range. It didn't have to be that way ... – PowerPoint PPT presentation

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Title: Nuclear Physics and the New Standard Model


1
Nuclear Physics and the New Standard Model
M.J. Ramsey-Musolf Wisconsin-Madison
NPAC
Theoretical Nuclear, Particle, Astrophysics
Cosmology
http//www.physics.wisc.edu/groups/particle-theory
/
Taiwan , June 2008
2
The Big Picture
Solar ns the neutrino revolution
Fifty years of PV in nuclear physics
3
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 !

4
Outline
  1. Overview Motivation
  2. Illustrative Scenario Supersymmetry
  3. Neutrinos Lepton Number ????
  4. EDMs the Origin of Matter
  5. Electroweak Precision Observables
  6. Weak Decays
  7. Neutral Current Processes

5
References
  • Low Energy Precision Test of Supersymmetry,
  • M.J. Ramsey-Musolf S. Su, Phys.Rept.456188,
    2008, e-Print hep-ph/0612057Model
  • Low energy tests of the weak interaction, J.
    Erler M. J. Ramsey-Musolf , Prog.Part.Nucl.Phys.
    54351 442, 2005, e-Print hep-ph/0404291

Plus many references therein
6
Motivation
  • Why New Symmetries ?
  • Why Low Energy Probes ?

7
Fundamental Symmetries Cosmic History
8
Fundamental Symmetries Cosmic History
9
Fundamental Symmetries Cosmic History
10
Fundamental Symmetries Cosmic History
Puzzles the Standard Model cant solve
  1. Origin of matter
  2. Unification gravity
  3. Weak scale stability
  4. Neutrinos

What are the symmetries (forces) of the early
universe beyond those of the SM?
11
Fundamental Symmetries Cosmic History
Baryogenesis When? CPV? SUSY? Neutrinos?
WIMPy D.M. Related to baryogenesis?
New gravity? Lorentz violation? Grav baryogen ?
?
12
Fundamental Symmetries Cosmic History
13
Fundamental Symmetries Cosmic History
14
Fundamental Symmetries Cosmic History
15
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

16
What are the new fundamental symmetries?
Two frontiers in the search
Collider experiments (pp, ee-, etc) at higher
energies (E gtgt MZ)
Indirect searches at lower energies (E lt MZ) but
high precision
Particle, nuclear atomic physics
High energy physics
17
Precision Probes of New Symmetries
New Symmetries
  1. Origin of Matter
  2. Unification gravity
  3. Weak scale stability
  4. Neutrinos

18
Precision Energy Frontiers
J. Ellison, UCI
19
Precision, low energy measurements can probe for
new symmetries in the desert
20
II. Illustrative Case SUSY
  • Why Supersymmetry ?
  • Key Features of SUSY

21
Couplings unify with SUSY
Supersymmetry
22
GF is Too Large
23
SUSY protects GF
24
GF the hierarchy problem
SUSY Relation
Quadratic divergence ?UV2 cancels
After EWSB
25
SUSY may help explain observed abundance of matter
Cold Dark Matter Candidate
Baryonic matter electroweak phase transition
26
SUSY a candidate symmetry of the early Universe
  • Unify all forces
  • Protect GF from shrinking
  • Produce all the matter that exists

3 of 4 Yes Maybe so
Maybe Probably necessary
  • Account for neutrino properties
  • Give self-consistent quantum gravity

27
Minimal Supersymmetric Standard Model (MSSM)
28
SUSY and R Parity
Consequences
29
R-Parity Violation (RPV)
?L1
WRPV ?ijk LiLjEk ??ijk LiQjDk ?/i LiHu
???ijkUiDjDk
?B1
proton decay Set ???ijk 0
30
Four-fermion Operators
31
SUSY must be a broken symmetry
32
MSSM SUSY Breaking
33
MSSM SUSY Breaking Models I
Gravity-Mediated (mSUGRA)
34
MSSM SUSY Breaking Models II
Gauge-Mediated (GMSB)
35
MSSM SUSY Breaking Models III
Parameter evolution mass
36
Gaugino-Higgsino Mixing
Chargino Mass Matrix
Neutralino Mass Matrix
37
Relic Abundance of SUSY DM
Neutralino Mass Matrix
38
Sfermion Mixing
Sfermion mass matrix
39
Test
100 new parameters 40 new CPV phases Flavor
mixing parameters
No new coupling constants
Two Higgs vevs
Supersymmetric Higgs mass, ?
40
Neutral Current Interactions II
Neutral current lf --gt lf at one loop
Normalization
Vector axial vector couplings
Weak mixing
41
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42
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