masato yamanaka (saitama university)
DESCRIPTION
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. Phys.Rev.D76:043528,2007. Introduction. - PowerPoint PPT PresentationTRANSCRIPT
Masato Yamanaka (Saitama University)
collaborators
Shigeki Matsumoto Joe Sato Masato Senami
Phys.Rev.D76:043528,2007Phys.Lett.B647:466-471 and
Relic abundance of dark matter in universal extra dimension models
with right-handed neutrinos
Introduction
What is dark matter ?
http://map.gsfc.nasa.govSupersymmetric modelLittle Higgs model
Is there beyond the Standard Model ?
Universal Extra Dimension model (UED model) Appelquist, Cheng, Dobrescu PRD67 (2000)
Contents of today’s talk
Solving the problems in UED modelsCalculation of dark matter relic abundance
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
Problems in Universal Extra Dimension (UED) model 1
UED models had been constructed as minimal extension of the standard model
Neutrinos are regarded as massless
We must introduce the neutrino mass into the UED models !!
Problems in Universal Extra Dimension (UED) model 2
Lightest KK Particle
Next Lightest KK particle
G (1)KK graviton
KK photon (1)KK parity conservation at each vertex
Lightest KK Particle, i.e., KK graviton is stable and can be dark matter
(c.f. R-parity and the LSP in SUSY)
Dark matter production(1) G (1)
high energy SM photon emission
It is forbidden by the observation !
Late time decay due to gravitational interaction
Solving the problems
Introducing the right-handed neutrino N
m N(1)
R1
+ 1/Rm 2
~ orderThe mass of the KK
right-handed neutrino N(1)
Dirac type with tiny Yukawa couplingMass type
Lightest KK Particle
Next to Next Lightest KK particle
G (1)KK graviton
KK photon (1)
Next Lightest KK particle KK right-handedneutrino N
(1)
Solving the problems
Branching ratio of the decay( 1)
Br( )( 1) =
( N )(1) (1)
( G )( 1)
(1) = - 75 × 10
New decay mode of :( 1)
( 1)
N
(1)
Neutrino masses are introduced into UED models, and problematic high energy photon emission is highly suppressed !!
stable, neutral, massive,weakly interaction
KK right handed neutrino can be dark matter !
Change of dark matter
After introducing the neutrino mass into UED models
Before introducing the neutrino mass into UED models
Dark matter KK graviton
Dark matter KK right-handed neutrino N
(1)
G(1)
decay allowed by KK parityN (1)
G (1)N
(1) N
m N(1) m + mG(1) (0)N<Forbidden by kinematics
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 !
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)
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 boson
KK gauge bosonKK fermionFermion mass term ( (yukawa coupling) (vev) )~ ・
t
x
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 ~ ・
N production needs processes including KK Higgs(n)
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
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
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 boson
KK gauge bosonKK fermionFermion mass term ( (yukawa coupling) (vev) )~ ・
t
x
Dominant N production process
(n)
UED model withright-handed neutrino
UED model withoutright-handed neutrino
Allowed parameter region changed much !!
[ Kakizaki, Matsumoto, Senami PRD74(2006) ]
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)
Summary
We have shown that after introducing neutrino masses, the dark matter is the KK right-handed neutrino, and we have calculated the relic abundance of the KK right-handed neutrino dark matter
In the UED model with right-handed neutrinos, the compactification scale of the extra dimension 1/R can be less than 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.
We have solved two problems in UED models (absence of the neutrino mass, forbidden energetic photon emission) by introducing the right-handed neutrino
Appendix
KK parity
(3)
(1)
φ (2)
(1)
(0)
(0)
φ
5th dimension momentum conservationQuantization of momentum by compactification
P = n/R5 R : S radius n : 0, 1, 2,….1
KK number (= n) conservation at each vertex
KK-parity conservation
n = 0,2,4,… + 1n = 1,3,5,… - 1
At each vertex the product of the KK parity is conserved
t
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) ]
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)
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)
= 2×10 [sec ]- 9 - 1 500GeV
( 1)
m3 m
10 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)
= 10 [sec ]- 15 - 1
3
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) ]
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
Boltzmann equation
dTdY
(n)
=s T Hm
C(m)(n)
1 +dT
dg (T)*s
3g (T)s*
T
C(m)(n)
= 4 g (2)3d k3 (m)
(m)N(n)
f(m)< 1 ー f >
L
s, H, g , f : entropy density, Hubble parameter, relativistic degree of freedom, distribution function
*s
Relic abundance calculation
g= 3= 2= 1 The normal hierarchy
The inverted hierarchyThe degenerate hierarchy
Y(n) = ( number density of N ) ( entropy density )(n)
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) ]