edm lhc ewb09a

7/29/2019 Edm Lhc Ewb09a

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EDMs, the LHC, and theOrigin of Matter

M.J. Ramsey-Musolf

Wisconsin-MadisonQuickTime and aTIFF (Uncomp ressed) decompresso

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http://www.physics.wisc.edu/groups/particle-theory/

NPACTheoretical Nuclear, Particle, Astrophysics & Cosmology

NC State Seminar, March 2009


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What is the origin of baryonic matter ?

Cosmic Energy Budget

Baryons

Dark Matter

Dark Energy

Explaining non-zerorBrequires CP-violationand a scalar sector beyond those of the

Standard Model(assuming inflation setrB=0)

What are the implications of Higgs searchesat LHC and Higgs studies at ILC for

explaining the baryon asymmetry ?

What are thequantitativeimplications of newEDM experiments for explaining the origin of

the baryonic component of the Universe ?

Leptogenesis: discoverthe ingredients:LN- & CP-violation in neutrinos

Weak scale baryogenesis:test experimentally:EDMs& Higgs Boson Searches

D. Chung Wisconsin

V. Cirigliano LANLB. Garbrecht Wisconsin

C. Lee LBL

Y. Li Wisconsin

S. Profumo UC Santa Cruz

S. Tulin Caltech

G. Shaugnessy Wisconsin

PRD 71: 075010 (2005)PRD 73: 115009 (2006)JHEP 0607:002 (2006 )PRD 78:075009 (2008)PRL 102:061301 (2009)

PLB 673: 95 (2009)

Baryogenesis & EDMs Higgs Phenomenology

PRD 75: 037701 (2007)JHEP 0807:010

(2007) PRD 77: 035005(2008) PRD79: 015018 (2009)

V. Barger Wisconsin

P. Langacker IASM. McCaskey Wisconsin

D. OConnell IAS

S. Profumo UC Santa Cruz

G. Shaugnessy ANL/Northwestern

M. Wise Caltech


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Outline

I. Baryogenesis: General Features

II. Preview of main results

III. Computing YBsystematically:progress & challenges

IV. Illustrative phenomenology inMSSM: EDMs & the LHC


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I. Baryogenesis: General Features


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Baryogenesis: Ingredients

Anomalous B-violating processes

Prevent washout by inverse processes

Sakharov Criteria

B violation

C & CP violation

Nonequilibriumdynamics

Sakharov, 1967

SM Sphalerons:

SM CKM CPV:

SM EWPT:

EDMs

LHC: Scalars


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EW Baryogenesis: Standard Model

Weak Scale Baryogenesis

B violation

C & CP violation


Sakharov, 1967

Anomalous Processes

Different vacua: D(B+L)= DNCS

A

Kuzmin, Rubakov, ShaposhnikovMcLerran,

Sphaleron Transitions

W

W

J

B

qL


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EW Baryogenesis: Standard Model


B violation

C & CP violation


Sakharov, 1967

mt4

MW4

mb4

MW4

mc2

MW2

ms2

MW2 31013

Js12s13s23c12c132 c23sin13

(2.88 0.33) 105

F

F

Increasing mh

1st order 2nd order

CP-violation too weak

No EWPT

Shaposhnikov


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Baryogenesis: New Electroweak Physics


B violation

C & CP violation

Nonequilibrium

dynamics

Sakharov, 1967

ne

(x)

Unbroken phase

Broken phaseCP Violation

Topological transitions

1st order phase transition

e

ne

ne

ne

g

g

e

e

Z0

Z0

Is it viable?

Can experiment constrain it?

How reliably can we compute it?

Quantum Transport

CPV

Chem Eq

R-M et al

Is it viable?

Can experiment constrain it?

How reliably can we compute it?

Theoretical Issues:Strength of phase transition (Higgs

sector) Bubble dynamics (numerical)

Transport at phase boundary (non-eq QFT)

EDMs: many-body physics & QCD

Systematic baryogenesis: SD

equations + power counting

Veff(,T):Requirements on Higgssector extensions & exptl probes

EDM sensitivity to CPVphases relevant for EWB:leptonic, hadronic, & nuclear


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EDMs: New CPV?

SM backgroundwell below newCPV expectations

New expts: 102to103more sensitive

CPV needed forBAU?

CKM


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Baryogenesis: EDMs & Colliders

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Cosmology LHC

EDMs

Theory

Theory

Implications


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EDMs & EWB: What We May Learn

Present n-EDM limitProposed n-EDM limit

?

Matter-AntimatterAsymmetry inthe Universe

Better theory ?New theory ?Leptogenesis ?

n-EDM has killedmore theories than

any othersingleexperiment


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II. Preview: Main Results


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MSSM Baryogenesis: EDMs & LHC

Resonant EWB

Present de

LEP II excl

LHC reach

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are needed to see this picture.

Prospective dn

Cirigliano, Profumo, R-M

+-driven EWB

0-driven EWB


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Probing the CPV Phase Structure

Arg(M1b*) = Arg(M2b

*)/

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Res EWB notcompatible with dn

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decompressorare needed to see this p icture.

Res & non-res

EWB compatiblewith future dn

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Li, Profumo, Ramsey-Musolf

Compatible with

observed YB

New 2-loop EDM calc


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YB& Particle Spectrum: LHC & g-2


are needed to s ee this picture.

Chung,Garbrecht, Ramsey-Musolf, Tulin

Small tan

Large tan

YBdependence on third generation

sparticle masses & tan

Magnitude & sign of YBsensitive to third generationsfermion spectrum for given CPV phase


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III. Computing YB


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Systematic Baryogenesis

Goal:Derive dependence of YB

on parametersLnewsystematically (controlled approximations)

Parameters inLnewBubble & PT

dynamics

CPV phases

Departure from equilibrium

Earliest work: QM scattering & stat mech

New developments: non-equilibrium QFT


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Systematic Baryogenesis

Unbroken phase

Topological transitions

Broken phase

1st order phase transition

(x)

rBt

D2rB WSFWS(x) nL (x)RrB

FWS(x) ->0 deep inside bubble

nL produced in wall& diffuses in front

Cohen, Kaplan,

NelsonJoyce, Prokopec,Turok

snow

W W

JB

qL

nL produced on short timescale compared to WS nL to

rBconversion


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Quantum Transport & Baryogenesis

Particle Propagation: Beyond familiar (Peskin) QFT

0IN

0OUT

LI

Assumptions: 1. Evolution is adiabatic2. Spectrum is non-degenerate

3. Density is zero

ne

(x)

Electroweak Baryogenesis 1. Evolution is non-adiabatic:vwall> 0 -> decoherence

2. Spectrum is degenerate:

T > 0 -> Quasiparticles mix3. Density is non-zero


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Quantum Transport & Baryogenesis

ne

(x)

Electroweak Baryogenesis 1. Evolution is non-adiabatic:

vwall> 0 -> decoherence

2. Spectrum is degenerate:

T > 0 -> Quasiparticles mix3. Density is non-zero

Scale Hierarchy:

Fast, but not too fast

Hot, but not too hot

Dense, but not too dense

d=vw(k /w)


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Quantum Transport Equations

= + +

G

G0

+

G0

G0

Expandind,p,

Currents

CP violating

sourcesLinks CP violation in Higgs

and baryon sectors

Chiral

Relaxation

Strongsphalerons

Producing nL = 0

SCPV

M, H , Y, SS

Xj(X) d

3z dz0 (X,z)G(z,X) G(X,z) (z,X)

X0ApproximationsNeglect O(3) terms

Others under scrutiny

R-M, Chung, Tulin,

Garbrecht, Lee,Cirigliano

From S-D Equations:SCPV

M, H, Y

Riotto, Carena et al, R-M et al,Konstandin et al

R-M et al

Objectives:

Determine param dep of SCPVand alls and not just that of SCPV

Develop general methods for anymodel with new CPV

Quantify theor uncertainties

Y>> other rates? (No)

Majorana fermions ?

(densities decouple) Particle-sparticle eq?

Vev resummation ?


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Our Work Applied to MSSM

Resonant enhancements in chiralrelaxation offsets resonant CPV

Three-body contributions enhance

Yukawa rates Large tan (g-2) regime quenches

YBand introduces strongdependence on SUSY spectrum

EDM constraints imply non-universalgaugino phases


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Illustrative Study: MSSM

Neutralino Mass Matrix

M1

-M2

-mZ cossinqW mZ coscosqWmZ sinsinqW -mZ sinsinqW 0

0

00

--mZ cossinqW mZ coscosqWmZ sinsinqW -mZ sinsinqWMN =

Chargino Mass Matrix

M2

MC =

cos2mW

sin2mW T


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Baryon Number: MSSM

YB rBs

F1 sin F2 sin( A )

F1S

H

CPV

WS

diff

F2St

CPV

WS

diff

Higgsinos SquarksImpt to computeboth num and denconsistently

F2: EWPO imply

suppression


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Resonant CPV & Relaxation

SH

R

(GeV)

(GeV)

MW

Huet &Nelson

MW

CP violation Relaxation

F1S

H

CPV

WS

diff


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Baryon Number & Y

Cirigliano, Lee, R-M, Tulin

gH

tLtLtR

Joyce, Prokopec, Turok

YB rBs

F1 sin F2 sin( A )

YB rB

sF1 sin F2 sin( A )

ourY

previous Y


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Baryogenesis: tan effectsTransport, Spectrum, & EDMs

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Canceling t,b (s)quarkcontributions

Enhanced light staucontributions



Small tan:nleft=5Q+4T



+ SUSYChung,Garbrecht, R-M, Tulin: PRL 102:061301 (2009)

QuickTime and a


Small tannegligible Yb,

effectstan=20: impt Yb,

effectsSmall tan: strong sphaleronsinduce 1st& 2ndgen quarkcontributions to counteract 3rdgeneration chiral asymmetry

Large tan: 3rdgeneration chiralasymmetry vanishes: no strongsphaleron-induced 1st& 2ndgenquark contributions


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IV. Phenomenology: EDMs, LHC, & YB


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EDMs: Complementary Searches

f

0

f

f

g

q

0

q

q

ElectronImprovementsof 102 to 103

Neutron

f

0

f

f

Neutral

Atoms

g

q

0

q

q

Deuteron

g

q

0

q

q

N

e

QCD

QCD

QCD


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EDMs: Theory

g

q

0

q

q

f

0

f

f

ElectronImprovementsof 102 to 103

Neutron

f

0

f

f

Neutral

Atoms

g

q

0

q

q

Deuteron

g

q

0

q

q

N

e

QCD

QCD

QCD

n

p

Nuclear Schiff Moment

Nuclear EDM:Screened in atoms

Neutron EDM from LQCD:

Two approaches:

Expand inq& average overtopological sectors (Blum et al,Shintani et al)

ComputeDE for spin up/downnucleon in backgroundEfield

(Shintani et al)

mN=2.2 GeV

QCD SR (Pospelov et al)

Hadronic couplings

Pospelov et al:

PCAC + hadmodels & QCD SR

ChPT for dn: van Kolck et al

Schiff Screening

Atomic effect fromnuclear finite size:Schiff moment


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EDMs & Schiff Moments

f

0

f

f

g

q

0

q

q

One-loop

EDM: q, l, n Chromo-EDM: q, n

Dominant innuclei & atoms

Engel & de Jesus:Reduced isoscalar sensitivity (qQCD)

Schiff Moment in199Hg Nuclear & hadron structure

Liu et al:New formulation of Schiff operator

+

New nuclear calcs needed


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One Loop EDMs & Baryogenesis

g

q

0

q

q

f

0

f

f

ne

(x)

q , W, B , Hu,d

T ~ TEW

Resonant Non-resonantCirigliano, Lee,Tulin, R-M

Futured

ed

nd

A


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EDMs in SUSY

f

0

f

f

g

q

0

q

q

One-loop




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EDMs in SUSY

f

0

f

f

g

q

0

q

q

One-loop



Two-loop

EDM only: no chromo-EDM

g

g

g

Weinberg: small matrix els

Decouple in large limit


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EDM constraints & SUSY CPV

AMSB: M1

~ 3M2

Baryogenesis

LEP II Exclusion

Two loop de

Cirigliano,

Profumo, R-MSUGRA: M

2

~ 2M1

| sin | > 0.02

| de, dn| > 10-28e-cm

M < 1 TeV

Arg(M1b*) = Arg(M2b

*)

+-driven EWB

0-driven EWB


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MSSM Baryogenesis: EDMs & LHC

baryogenesis

Present de

LEP II excl

LHC reach

QuickTime and aTIFF (Uncompressed) decompressor


Prospective dn

Cirigliano, Profumo, R-M

+-driven EWB

0-driven EWB


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EDMs in SUSY: Full Two-Loop

Higgs Boson Masses

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decompressorare needed to see t his picture.

Li, Profumo, R-M: PRD 78:075009(2008)

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WH Loops dominate for neutron &comparable toH, A for electron

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mA=300 GeV, =300 GeV, M2=2M1=290 GeV


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EDMs in SUSY: Full Two-Loop

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Higgs Boson Masses

Stronger limits onCPV for lightHiggses & large tan

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Arg(M1b*) = Arg(M2b

*)


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Baryogenesis: EDMs & LHC

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Higgs Boson MassesQuickTime and a


Stronger limits onCPV for lightHiggses & large tan

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Examples w/ mstop= 125 GeV,mA=200 GeV:tan=15, sin=0.05; tan~5, sin=0.1

Large tan(g-2) & universal gauginoCPVchallenging for MSSM EWB

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EDMs & EWB: Non-universal phases

Arg(M1b*) = Arg(M2b

*)/

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Weak dependence ofde, dnon Arg(M1b

*)


are needed to see t his picture.

Res EWB notcompatible with dn

QuickTime and a

decompressorare needed to see this p icture.

Res & non-res

EWB compatiblewith future dn, lightmA, & moderatetan

Li, Profumo, R-M: PLB673:95 (2009)


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Summary

EWB remains a viable and testablescenario for explaining the cosmicbaryon asymmetry

We are making progress in refining YB& EDM computations with reducedtheoretical uncertainties

Input from EDM searches, colliderstudies, & theory needed to addressthe origin of matter problem

edm lhc ewb09a

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