Sussex 22.8.2007

The WIMP of a minimal walking Technicolor Theory

J. VirkajärviJyväskylä University, Finland

with K.Kainulainen and

K.Tuominen

Outline• Technicolor and the WIMP

• Dynamical Dark Energy and the WIMP density

• Model results

• Conclusion & outlook

Basic idea of Technicolor (TC)

Technifermion condensate = a composite Higgs

(+ (pseudo) Goldstone bosons)

• New gauge interaction TC which only technifermions feel

• Left and right handed fermions (massless) have SU(2) chiral symmetry

• Spontaneus symmetry breaking dynamicallyElectroweak symmetry breakingRight mass ratio for EW gauge bosons

Early UniverseHigh TemperatureT > TeV

Universe expands,T drops

GeVTEW 175

• Model: Two techniquarks(flavors) in two index symmetric (= adjoint) presentation of an SU(2) TC gauge group.

• Witten anomaly cured by introducing a new Heavy lepton family

Minimal Walking TC (WTC)

2121 ,, , ccR

ccR DU

L

cc

cc

D

U

},{

},{

21

21

LN

Heavy Neutrino = the WIMP

• Near conformal (=walking) FCNC’s suppressed.

• Compatible with EW precision measurements

(Sannino & Tuominen, hep-ph/0405209)

(Pure Majorana case)

Heavy neutrino mass term• Dirac mass term for charged lepton

• For neutrino three cases:

1. Pure Dirac mass term ( )

2. Pure Majorana mass term (M)

3. Mixed Dirac-Majorana mass term:

..0

2 chm

mML C

R

L

D

DR

CLmass

Thermally averaged annihilation cross section:

MAJORANAPURENMIXED vv 4)( sin

1

decays to = the WIMP 2N 1N

Diagonalize two Majorana particles: and (mass eigenstates) for which and21 mm

1N 2N

Dm

EW precision measurements

Neutrino

Charged lepton

• Model consistent with data (hep-ex/0509008) .• Oblique parameters S and T (Peskin & Takeuchi, PRD 46 (1992)).

Pure Majorana

12 2 mm Similar results in Pure Dirac and mixed cases

• Quintessence:

• Dark energy dominates the energy density at early times

Dynamical Dark Energy

• Dark Energy

• Dark Matter

• Baryonic Matter

20.0~N

76.0~

04.0~B

)(2

1QVQQLQ

0)(33

QH

QVQHQ

63 i.e. aaQ Q 4 arad SM only radiation

”0” means T = 1MeV

• Relic density from Lee Weinberg equation

• Biggest effects to final abundance of the heavy neutrinos comes from the cross section and Hubble parameter

)()()( 2

eq2

2

xfxfH

xmv

x

xf N

Exponentialdrop

Freeze out

Relic density and dynamical dark energy

)()()( 2

eq2

2

xfxfH

xmv

x

xf N

Number density

3*

23/1

)(45

2 , ,

)()( TTgs

m

sx

s

xnxf

N

SUSY and Our mixed D-M mass case

Our Model

6

0

4

00,3

8

a

ar

a

ah

GH rad

N

”0” means T = 1 MeV

6 aQ4 aradSM

0,

0,

rad

Qr

Model results

contours const.~N

)0(1009.1 6 famNN

Both cases compatible with nucleosynthesis since r small (for masses shown).

Pure Dirac Pure Majorana

Majoranafor 2

1

Diracfor 1

a

a

Model resultsMixed Dirac-majorana case:

410rDotted:

Dashed: 710r

Solid: Standard expansion

0r

contours const.~N

2

32

4 41sin308,0

Zm

mN

Yellow areaExcluded by LEP:

Similar results by Kouvaris:(hep-ph/0703266)for neutral bound state betweentechniquark and technigluon

Constraints to results• Direct search limits

Bound depends on the ratio between local and cosmic WIMP densities

0/ nnk G

• Limit from rotation curves + halo models: lower bound for local density 3

06.0cm

GeVG

(Jungman, Kamionkowski, Griest, Phys. Rept. 267)

Pure DiracPure Majorana,(mixed D-M)Upper limits for ),( kmNN

Conclusion and outlook• If a Quintessence-like Dark Energy dominates the early

universe evolution– 4th generation dirac neutrino (from MWTC) with m < 800 GeV is excluded– Majorana neutrino with m > 100 GeV candidate for dark matter: not excluded by direct searches

• In standard expansion case from mixed Majorana-Dirac mass term– Mainly right handed Majorana neutrino with m > 23 GeV candidate

for dark matter: not excluded by LEP or direct searches.

• Further studies:– Other CDM in extensions of MWTC– Replacing Quintessence with more advanced DE models