masato yamanaka (saitama university)

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Masato Yamanaka (Saitama University) collabora tors Shigeki Matsumoto Joe Sato M asato Senami arXiv:0705.0934 [hep -ph] Phys.Lett.B647:466-471 and Relic abundance of dark matter in universal extra dimension models with right-handed neutrinos (To appear in PRD)

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Relic abundance of dark matter in universal extra dimension models with right-handed neutrinos. Masato Yamanaka (Saitama University). collaborators. Shigeki Matsumoto Joe Sato Masato Senami. Phys.Lett.B647:466-471 and. arXiv:0705.0934 [hep-ph]. (To appear in PRD). Introduction. - PowerPoint PPT Presentation

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Page 1: Masato Yamanaka (Saitama University)

Masato Yamanaka (Saitama University)collaborators

Shigeki Matsumoto Joe Sato Masato Senami

arXiv:0705.0934 [hep-ph] Phys.Lett.B647:466-471 and

Relic abundance of dark matter in universal extra dimension models

with right-handed neutrinos

(To appear in PRD)

Page 2: Masato Yamanaka (Saitama University)

Introduction

What is dark matter ?

http://map.gsfc.nasa.govSupersymmetric modelLittle Higgs model

Is there beyond the Standard Model ?

(1) Construction of problemless UED model (2) Calculation of dark matter relic abundance

Universal Extra Dimension model (UED model) Appelquist, Cheng, Dobrescu PRD67 (2000)

Contents of today’s talk

Page 3: Masato Yamanaka (Saitama University)

What is Universal

5-dimensions

compactified on an S /Z orbifold1 2

all SM particles propagatespatial extra dimension

(time 1 + space 4)

Extra Dimension (UED) model ?

R

4 dimension spacetime

S1

(1)

Standard model particle (2), , ,‥‥ (n)

KK particle

KK particle mass : m = ( n /R + m + m )(n) 222

m : corresponding SM particle mass2SM

1/2SM

2

m : radiative correction

Page 4: Masato Yamanaka (Saitama University)

For 1/R < 800 GeV~For 1/R > 800 GeV~

NLKP : (1)

NLKP : G (1)

LKP : G (1)

LKP : (1)LKP :

&Who is dark matter ?

KK parity

KK parity conservation at each vertexLightest Kaluza-Klein Particle(LKP) is stable and can be dark matter

(c.f. R-parity and the LSP in SUSY)

Dark matter candidate

Possible NLKP decayNLKP LKP + SM particle

NLKP : Next Lightest Kaluza-Klein Particle

Page 5: Masato Yamanaka (Saitama University)

Problems in Universal Extra Dimension (UED) model

Allowed

[ Kakizaki, Matsumoto, Senami PRD74(2006) ]

(1) The absence of the neutrino mass

(2) The diffuse photon from the KK photon decay

KK photon (from thermal bath)

Late time decay into KK graviton and high energy SM photon

It is forbidden by

the observation !

Excluded

Page 6: Masato Yamanaka (Saitama University)

Solving the two problems

Before introducing Dirac neutrinom G(1)> m(1)

Problematic is always emitted from decay(1)

After introducing Dirac neutrinom G> m> m (1)N (1)

(1)

New decay channels open !!(1)

Introducing the right-handed neutrino N

m N(1)R1 + 1/R

m 2~ order The mass of the KK right-handed neutrino N(1)

Page 7: Masato Yamanaka (Saitama University)

Br( )( 1) =( N )(1) (1)

= 5 × 10 500GeV3

m0.1 eV- 7

2 m1 GeV

1 / R

Presence of neutrino massAbsence of the diffuse photon problem

We have created the realistic UED model

Allowed !!

( G )

Branching ratio of the decay( 1)

( 1) (1)

Page 8: Masato Yamanaka (Saitama University)

(1)

G(1)

N (1)

N (0)

N decay is impossible ! (1)

stable, neutral, massive, weakly interactionKK right handed neutrino can be dark matter !

m N(1)R1 + 1/R

m2~ order

Change of DM (for 1/R < 800GeV) :G(1) N (1)

Who is dark matter ??

Br( )( 1) =( N )(1) (1)

( G DM production process ) ~ 10- 7

< m + mG(1) (0)N

Page 9: Masato Yamanaka (Saitama University)

G(1) : Almost produced from decay(1)

N (1) (1)

When dark matter changes from G to N , what happens ?

(1)(1)

: Produced from decay and from thermal bath

Additional contribution to relic abundance

Total DM number density

DM mass ( ~ 1/R )

We must re-evaluate the DM number density !

Page 10: Masato Yamanaka (Saitama University)

1 From decoupled decay (1) (1) N(1)

2 From thermal bath (directly)

Thermal bath( 1)N

3 From thermal bath (indirectly)

Thermal bath( n)N Cascade

decay

( 1)N

( 1)N

Production processes of new dark matter N( 1)

Page 11: Masato Yamanaka (Saitama University)

N(n) Production process

In thermal bath, there are many N production processes(n)

N(n)N(n) N(n)

N(n) N(n)

KK Higgs bosonKK gauge bosonKK fermionFermion mass term ( (yukawa coupling) (vev) )~ ・

t

x

Page 12: Masato Yamanaka (Saitama University)

N(n) Production process

N(n)N(n) N(n)

t

x

In the early universe ( T > 200GeV ), vacuum expectation value = 0

(yukawa coupling) (vev) = 0 ~ ・

Page 13: Masato Yamanaka (Saitama University)

Thermal correction

The mass of a particle receives a correction by thermal effects, when the particle is immersed in the thermal bath.

[ P. Arnold and O. Espinosa (1993) , H. A. Weldon (1990) , etc ]

2m (T)Any particle mass = 2m (T=0) + m (T)2

m (T) ~ m ・ exp[ ー m / T ]

loop For m > 2Tloop

m (T) ~ T For m < 2Tloop

m loop : mass of particle contributing to the thermal correction

Page 14: Masato Yamanaka (Saitama University)

Thermal correction

KK Higgs boson mass

m (T) = m (T=0) + [ a(T) 3+x(T)3y ]

2 2h t2 2 T2

12(n)(n) ・・

x(T) = 2[2RT] + 1

[ ] : Gauss' notation‥‥

a(T) = m=0

∞θ 4T - m R ー 22 2 [ a(T) 3+x(T)3y

]h t2 2・・ T2

12

T : temperature of the universe : quartic coupling of the Higgs bosony : top yukawa coupling

Page 15: Masato Yamanaka (Saitama University)

N(n) Production process

In thermal bath, there are many N production processes(n)

N(n)N(n) N(n)

N(n) N(n)

KK Higgs bosonKK gauge bosonKK fermionFermion mass term ( (yukawa coupling) (vev) )~ ・

t

x

Dominant N production process

(n)

Page 16: Masato Yamanaka (Saitama University)

UED model withright-handed neutrino

UED model withoutright-handed neutrino

Allowed parameter region changed much !!Excluded

Page 17: Masato Yamanaka (Saitama University)

1/R can be less than 500 GeV In ILC experiment, can be produced !!n=2 KK particle

It is very important for discriminating UED from SUSY at collider experiment

Produced from decay (m = 0)

(1)

Produced from decay + from the thermal bath

(1)

Page 18: Masato Yamanaka (Saitama University)

Summary

We have solved two problems in Universal Extra Dimension (UED) models (absence of the neutrino mass, forbidden energetic photon emission), and constructed realistic UED model.

In constructed UED model, we have investigated the relic abundance of the dark matter KK right-handed neutrino

In the UED model with right-handed neutrinos, the compactification scale 1/R can be as large as 500 GeV

This fact has importance on the collider physics, in particular on future linear colliders, because first KK particles can be produced in a pair even if the center of mass energy is around 1 TeV.

Page 19: Masato Yamanaka (Saitama University)

Appendix

Page 20: Masato Yamanaka (Saitama University)

What is UniversalExtra Dimension (UED) model ?

Fifth-dimension is compactified on an S1 R

4 dimension spacetime

All SM particles has the excitation mode called Kaluza-Klein (KK) particle

(1)

Standard model particle (2), , ,‥‥ (n)

KK particle

S1

5-dimension spacetime

Page 21: Masato Yamanaka (Saitama University)

5th dimension momentum conservation For S compactification 1 P = n/R5

R : S radius n : 0, ±1, ±2,….1

KK number (= n) conservation at each vertexS1/ Z 2 orbifolding P = 5 P 5-

KK-parity conservation

n = 0,2,4,… + 1n = 1,3,5,… - 1At each vertex the product of the KK parity is conserved

(3)(1)

φ (2)

(1)(0)

(0)

KK parity

φ

Page 22: Masato Yamanaka (Saitama University)

m = R1

G(1)Mass of the KK graviton

Mass matrix of the U(1) and SU(2) gauge boson

: cut off scale v : vev of the Higgs field

Radiative correction[ Cheng, Matchev, Schmaltz PRD66 (2002) ]

Page 23: Masato Yamanaka (Saitama University)

Dependence of the ‘‘Weinberg’’ angle

[ Cheng, Matchev, Schmaltz (2002) ]

sin 2W~~ 0 due to 1/R >> (EW scale) in the

mass matrix

~~B(1) (1)

Page 24: Masato Yamanaka (Saitama University)

= 2×10 [sec ]- 9 - 1 500GeV( 1)m

3 m10 eV- 2

2 m1 GeV

2

m = mN( 1 )m - m : SM neutrino mass( 1 )

Decay rate for ( 1) N( 1)

Solving cosmological problemsby introducing Dirac neutrino

(1)N (1)

Page 25: Masato Yamanaka (Saitama University)

= 10 [sec ]- 15 - 13

1 GeVm´

m = m - m(1) G(1)

Decay rate for ( 1) G( 1)(1)

G(1)

Solving cosmological problemsby introducing Dirac neutrino

[ Feng, Rajaraman, Takayama PRD68(2003) ]

Page 26: Masato Yamanaka (Saitama University)

We expand the thermal correction for UED model

Thermal correction

We neglect the thermal correction to fermionsand to the Higgs boson from gauge bosons

Gauge bosons decouple from the thermal bath at once due to thermal correction

Higgs bosons in the loop diagrams receive thermal correctionIn order to evaluate the mass correction correctly,

we employ the resummation method[P. Arnold and O. Espinosa (1993) ]

The number of the particles contributing to the thermal mass is determined by the number of the particle lighter than 2T

Page 27: Masato Yamanaka (Saitama University)

Result and discussion

N abundance from Higgs decay depend on the y (m )(n)

Degenerate case

m = 2.0 eV

[ K. Ichikawa, M.Fukugita and M. Kawasaki (2005) ]

[ M. Fukugita, K. Ichikawa, M. Kawasaki and O. Lahav (2006) ]

Page 28: Masato Yamanaka (Saitama University)

reheating temperature (1/R)

Nh21/R = 600 GeV

m = 120 GeVh

m = 0.66 eV

degenerate case

N abundance depends on the reheating temperature(n)

If we know 1/R and m , we can get the constraint for the reheating temperature

Page 29: Masato Yamanaka (Saitama University)

Solving cosmological problemsby introducing Dirac neutrino

We investigated some decay mode(1)

(1)N(1)

(1)

G(1)

(1)N(1)h(1)

llW

etc.

Dominant decay mode from (1)

Dominant photon emission decay mode from (1)

Page 30: Masato Yamanaka (Saitama University)

N(n) Production process

In thermal bath, there are many N production processes(n)

N(n)N(n) N(n) N(n) N(n)

N(n) N(n)

etc.

1/R > 400GeV ( from precision measurements )We concentrate on the early universe inT > 200 GeV for relic abundance calculation

There is no vacuum expectation value in the era

Many processes disappear