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M.J. Ramsey-Musolf. Sub Z Supersymmetry. Precision Electroweak Studies in Nuclear Physics. NSAC Long Range Plan. What is the structure of the nucleon? What is the structure of nucleonic matter? What are the properties of hot nuclear matter? What is the nuclear microphysics of the universe?

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sub z supersymmetry

M.J. Ramsey-Musolf

Sub Z Supersymmetry

Precision Electroweak Studies in Nuclear Physics

nsac long range plan
NSAC Long Range Plan
  • What is the structure of the nucleon?
  • What is the structure of nucleonic matter?
  • What are the properties of hot nuclear matter?
  • What is the nuclear microphysics of the universe?
  • What is to be the new Standard Model?

Neutrino physics

Precision measurements: -decay, -decay, parity violating electron scattering, EDM’s…

What can they teach us about the new Standard Model?

slide3

TheStandard Modelof particle physics is a triumph of late 20th century physics

  • It provides a unified framework for 3 of 4 (known) forces of nature in context of renormalizable gauge theory
slide4

TheStandard Modelof particle physics is a triumph of late 20th century physics

  • Utilizes a simple & elegant symmetry principle to organize what we’ve observed
slide5

TheStandard Modelof particle physics is a triumph of late 20th century physics

  • Utilizes a simple & elegant symmetry principle to organize what we’ve observed

Scaling violations in DIS Asymptotic freedom R(e+e-) Heavy quark systems Drell-Yan

Strong (QCD)

slide6

TheStandard Modelof particle physics is a triumph of late 20th century physics

  • Utilizes a simple & elegant symmetry principle to organize what we’ve observed

“Maximal” parity violation Conserved Vector Current CP-Violation in K, B mesons Quark flavor mixing Lepton universality…..

Electroweak (=weak + QED)

slide7

TheStandard Modelof particle physics is a triumph of late 20th century physics

  • Most of its predictions have been confirmed

Parity violation in neutral current processes: deep inelastic scattering, atomic transitions

slide8

sin2qW

The Standard Modelof particle physics is a triumph of late 20th century physics

  • Most of its predictions have been confirmed

Jl0

Jlg

JlY

JlZ

Neutral currents mix

slide9

Not yet!

TheStandard Modelof particle physics is a triumph of late 20th century physics

  • Most of its predictions have been confirmed
  • W, Z0
  • 3rd fermion generation (CP violation, anomaly)
  • Higgs boson

New particles should be found

we need a new standard model

Large Hadron Collider

Ultra cold neutrons

LANSCE, SNS, NIST

CERN

We need anew Standard Model

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

outline

Precision measurements

  • “Forbidden processes”
  • Weak decays
  • lepton scattering
Outline

SM Radiative Corrections & Precision Measurements

Defects in the Standard Model

An Example Scenario: Supersymmetry

Low-energy Probes of Supersymmetry

outline12

Precision measurements

  • “Forbidden processes”
  • EDM’s
  • 0nbb decay
  • m !e, m !eg…
Outline

SM Radiative Corrections & Precision Measurements

Defects in the Standard Model

An Example Scenario: Supersymmetry

Low-energy Probes of Supersymmetry

fermi s theory could incorporate higher order qed contributions
Fermi’s theory could incorporatehigher order QED contributions

QED radiative corrections: finite

the fermi theory has trouble with higher order weak contributions
The Fermi theory has trouble withhigher order weak contributions

Weak radiative corrections: infinite

Can’t be absorbed through suitable re-definition of GFin HEFF

all radiative corrections can be incorporated in the standard model with a finite number of terms

Re-define g

Finite

All radiative corrections can be incorporated in the Standard Model with afinitenumber of terms

g

g

g

g f encodes the effects of all higher order weak radiative corrections

g

g

GFencodes the effects of all higher orderweak radiative corrections

Drm depends on parameters of particles inside loops

comparing radiative corrections in different processes can probe particle spectrum

g

g

Comparingradiative corrections in different processes canprobeparticle spectrum

Drm differs from DrZ

comparing radiative corrections in different processes can probe particle spectrum21

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

Radiative corrections

Direct Measurements

Stunning SM Success

Comparingradiative corrections in different processes canprobeparticle spectrum

J. Ellison, UCI

collider studies

LEP

SLD

Tevatron

Collider Studies

R. Clare, UCR

collider studies25

MW

Mt

Am

shad

Collider Studies

Tevatron

ii why a new standard model
II.Why a “New Standard Model”?
  • There is no unification in the early SM Universe
  • The Fermi constant is inexplicably large
  • There shouldn’t be this much visible matter
  • There shouldn’t be this much invisible matter
the early sm universe had no unification32

Present universe

Early universe

Standard Model

High energy desert

Weak scale

Planck scale

The early SM Universe had nounification
the early sm universe had no unification33

Present universe

Early universe

Standard Model

Gravity

A “near miss” for grand unification

High energy desert

Weak scale

Planck scale

The early SM Universe had nounification
the fermi constant is too large

Present universe

Early universe

Unification Neutrino mass Dark Matter

Standard Model

GF would shrink

High energy desert

Weak scale

Planck scale

The Fermi constant is too large
a smaller g f would mean disaster

Smaller GF More 4He, C, O…

A smaller GF would mean disaster

The Sun would burn less brightly

G ~ GF2

Elemental abundances would change

Tfreeze out ~ GF-2/3

there is too much matter visible invisible in the sm universe

Measured abundances

SM baryogenesis

There is too much matter -visible & invisible - in the SM Universe

Visible Matter from Big Bang Nucleosynthesis

Insufficient CP violation in SM

there is too much matter visible invisible in the sm universe38

No SM candidate

Dark

Insufficient SM CP violation

Visible

There is too much matter -visible & invisible - in the SM Universe

Invisible Matter

S. Perlmutter

there must have been additional symmetries in the earlier universe to
There must have been additional symmetries in the earlier Universe to
  • Unify all forces
  • Protect GF from shrinking
  • Produce all the matter that exists
  • Account for neutrino properties
  • Give self-consistent quantum gravity
iii supersymmetry
III.Supersymmetry
  • Unify all forces
  • Protect GF from shrinking
  • Produce all the matter that exists

3 of 4

Yes

Maybe so

  • Account for neutrino properties
  • Give self-consistent quantum gravity

Maybe

Probably necessary

susy may be one of the symmetries of the early universe

Fermions

Bosons

sfermions

gauginos

Higgsinos

Charginos, neutralinos

SUSY may be one of the symmetries of the early Universe

Supersymmetry

couplings unify with susy

Present universe

Early universe

Standard Model

High energy desert

Weak scale

Planck scale

Couplings unify with SUSY

Supersymmetry

susy may help explain observed abundance of matter

c0 Lightest SUSY particle

CP Violation

Unbroken phase

Broken phase

SUSY may help explain observed abundance of matter

Cold Dark Matter Candidate

Baryonic matter

susy must be a broken symmetry

SUSY Breaking

Superpartners have not been seen

Theoretical models of SUSY breaking

Visible World

Hidden World

Flavor-blind mediation

SUSY must be a broken symmetry
minimal supersymmetric standard model mssm

LSM

LSM

+

LSUSY

+

Lsoft

Minimal Supersymmetric Standard Model (MSSM)

Lsoft gives

contains 105 new parameters

How is SUSY broken?

slide47

Visible Sector:

Hidden Sector: SUSY-breaking

MSSM

Flavor-blind mediation

How is SUSY broken?

Gravity-Mediated (mSUGRA)

slide48

Visible Sector:

Hidden Sector: SUSY-breaking

MSSM

messengers

How is SUSY broken?

Flavor-blind mediation

Gauge-Mediated (GMSB)

slide49

ln

gaugino mass

group structure

increases as

decreases

increases faster than

at the weak scale

Mass evolution

mssm and r parity
MSSM and R Parity

SM Particles:

Superpartners:

Matter Parity: An exact symmetry of the SM

mssm and r parity52
MSSM and R Parity

MSSM conserves

vertices have even number of superpartners

Consequences

  • Lightest SUSY particle

is stable

viable dark matter candidate

  • Proton is stable
  • Superpartners appear only in loops
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