ダークマターの候補粒子に対する宇宙物理・宇宙論的制限

Kazunori Kohri （郡和範）

Physics Department, Lancaster University

Contents• Brief review of Big-bang Nucleosynthesis (BBN)• Brief review of Supersymmetry (SUSY) and Supergravity(SUGRA)• Lightest SUSY Particle (LSP) Dark Matter (DM) in Minimal
SUSY Standard Model (MSSM), Constrained MSSM(CMSSM) and mSUGRA• Cosmological and astrophysical constraints on Lightest SUSY
Particle (LSP) and Next LSP (NLSP)• Solving lithium problem

Brief review ofBig-bang nucleosynthesis (BBN)Thermal history of the Universecf) 1 GeV ~ 1013K

Big bang
time
10
10

−44
−38

"temperature"sec − 10 GeV
18

sec − 10 GeV
16

10−11 sec − 102 GeV

Planck scale

Inflation and Reheating

GUT phase transition?
Electroweak phase transition

Baryogenesis?

− 200 MeV Neutrino decoupling− 3 MeV Electron-positron annihilation Big-Bang
Nucleosynthesis− 0.5 MeV
(BBN)
Matter-radiation equality
10 sec − 1 eV
Photon decoupling (CMB)
10 sec − 0.1 eV−5

QCD phase transition

10 sec0.1 sec
1 sec
10
12

≈

13.717Gyr − 10- 4 eV(~10 sec)

Present

Thermal history around BBN Epoch
10−4 sec−100 MeV

Muon annihilationcf) 100 MeV ~ 1012K( μ + + μ − → 2γ )≈0.1 sec
1 sec
2

10 sec103 sec− 2 -- 3 MeV Neutrino decoupling (ν + e ν + e )
(n +ν
p+e )
− 1 MeV n/p freezeout− 0.5 MeV Electron-positron annihilation(e + e → 2γ )− 0.1 MeV Beginning of BBN− 0.07 MeV End of (Standard) BBN
−

e

−

e

−

e

+

−

Scenario of BBNcf) 1 MeV ~ 1010K

1) T > 1 MeV (t < 1sec)
Radiation

γ , e ,νMattern, p±

Weak interaction is in equilibriumn + e ↔ p +ν e
+

nn
⎡ Q⎤
= Exp ⎢ − ⎥np⎣ T⎦(Q ≡ mn − m p ∼ 1.29 MeV)

2) T ~ 1 MeV (t ~ 1 sec) cf) 1 MeV ~ 10 K
10Feezeout of weak interaction•Weak interaction rate
•Hubble expansion rate

Γ n ↔ p ~ σ n ↔ p ne ~ GF2 T 5
H=

Γ ⎛
T
⎞
≈⎜
⎟
H ⎝ 0.8 MeV ⎠Γ < H (T < 0.8 MeV ≡ T f )a (t )~ T 2 / M pla (t )

3( n /n ) is fixed⎛ nn ⎞⎡ Q⎤≈ Exp ⎢ − ⎥⎜⎜ ⎟⎟⎝ n p ⎠freezeout⎣⎢ T f ⎦⎥np

He4 mass fraction⎛ nn ⎞1≈⎜⎜ ⎟⎟⎝ n p ⎠freezeout 7⎡ Q⎤
Exp ⎢ − ⎥
⎣ T⎦

4

n

He

p

n

p

n He = nn /2
4

ρ He 4 × mN × n He2(nn / n p )freezeout
Yp ≡≈≈≈ 0.25
ρB
mN × (nn + n p ) (nn / n p )freezeout +1
44cf) 0.1 MeV ~ 109K

3) T ~ 0.1 MeV (t ~ 100 sec)p + n → D +γ

T

BD = 2.2 MeV

4) T < 0.1 MeV (t > 100 sec)nD / nH ∼ 16.3(T / mN )3/ 2η exp[ BD / T ] > 0.01

D + D → T + p, 3 He+n
T + D ( 3 He + D) → 4 He+n ( 4 He+p)
A little D and 3 He are left as cold ashes

There is no stable nuclei for A=5,8. Mass 7 nuclei are produced a little.
4

He + T → 7 Li+γ4

He + 3 He → 7 Be+γ
7

4

He + D → 6 Li+γ

Be + e − → 7 Li+ν e

Time evolution of light elements

Observational light element abundances
41) He
zObserve the recombination line in Metal poor extragalactic H II region,or blue compact galaxyzIdentifying H II region as He II regionzExtrapolating them into zero metalicity

Yp = 0.250 ± 0.004
Fukugita, Kawasaki (06)Yp = 0.2474 ± 0.0028
Peimbert, Luridiana, Peimbert (07)Yp = 0.2516 ± 0.0011
Izotov, Thuan, Stasinska (07)Fukugita, Kawasaki (06)2) Deuterium
Observed in high redshift QSO absorption system

QSO
Lyα（z~3）
DH

D / H = (2.82 ± 0.26) ×10−5
O’Meara et al.(2006)

82km/sec

Burles and Tytler (1997)

2) Lithium 7
zObserving metal poor halo stars in Pop II
zAbundance does not depend on metalicity so much for

Teff > 5700 K ( ∝ M ), [Fe/H ] < -2

“Spite’s plateau”

L og10 ( 7Li/H ) = −9.90 ± 0.09
Bonifacio et al (2006)

Lemoine et al., 1997

Observational Light Element
Abundances
He4

Yp = 0.2516 ± 0.004

Fukugita, Kawasaki (2006)
Peimbert,Lridiana, Peimbert(2007)
Izotov,Thuan, Stasinska (2007)

D

D/H = (2.82 ± 0.26) × 10 −5Li7

log10 ( 7Li/H ) = −9.90 ± 0.09 ( ±0.35)syst.

Melendez,Ramirez(2004)

Li/ 7Li < 0.046 ± 0.022 ( ±0.106)sys

Asplund et al(2006)

Li6
He3

6

He /D < 0.83 + 0.27

3O’Meara et al. (2006)

Geiss and Gloeckler (2003)

SBBN(≡ nB / nγ )(≡ nB / nγ )

ηWMAP = (6.225 ± 0.160) × 10 −10

Brief review ofSupersymmetry (SUSY)

Dark Matter? Einstein’s Cosmological ConstantOr unknown scalar field?

Dark side?
ΩCDM h 2 ∼ 0.1

Dark
Side
96%

Dark side?
Unknown SUSY particles?

Light side (Baryon) 4%
http://map.gsfc.nasa.gov/media/060916

Realistic candidates of particle dark matter in
SUSY/SUGRA• Neutralino χ(Bino, wino, or higgsinos)
Most famous Lightest SupersymmetricParticle (LSP) with mχ~100GeV (appears
even in global SUSY)• Gravitino ψμsuper partner of graviton with spin 3/2
and m3/2 < 100GeV (massive only in
SUGRA (local SUSY))Introduction to SUSY
Supersymmetry (SUSY)
Solving “Hierarchy Problem”
Realizing “Coupling constant unification in GUT”

neutralino

Fermion

Boson

quark

squarkleptonsleptonphotinophotongravitino

graviton

axino

axion

Highly model-dependentand my review isinsufficient
See Kawasaki, Senami,
Nakayama (07)Depending on SUGRA models

Hierarchy Problems
GUT-scaleMX ≈ 1014 - 1015GeV

12-13 orders ofmagnitude !!!

Weak-scale

MW ≈ 10 -10 GeV
2

Higgs mass

3

2
d
Vϕ
2
2
2
mϕ 0 =
O
M
≈
λ
υ
≈
(
W )
2
dϕ

Vϕ

where Higgs’s potential

Vϕ = λ (ϕ ϕ − υ /2 )†22c.f) Masses of fermions and vector bosonsmψ ~ hψ ϕ , mZ ~ g ϕ~υ ϕRadiative correction to Higgs massin Quantum Field Theory
W

ϕ
ϕ

+
λ

ϕ

ϕ

δ mϕ2 ~ λΛ2 + g 2 Λ2g ϕ

g

Quadratic divergence

Cut off scale Λ ~ MX ~ 1015 GeV

δ mϕ ~ (10 GeV ) ?
2

15

2

How can we resolve the problem?
Weak scale in the tree level,~ (10 GeV )

m

2
ϕ0

2

2

δ mϕ ~ (10 GeV )2

In total,

15

2

mϕ ~ mϕ 0 + δ mϕ ~ (10 GeV ) ?
2

2

2

15

2

To retain the hierarchy, we require an accidental cancellation,

mϕ 0 + δ mϕ 1 + δ mϕ 2 + δ m + ... ~ (10 GeV ) ?
2

2

2

2
ϕ3

⎡⎣O (10 GeV) ⎤⎦15

GDP in USA (2002)?

2

2$ 10,110,087,734,958.95-) $ 10,110,087,734,957.70$ 1.25Fine tuning!

2Solution in SUSY
In exact SUSY, the quadratic divergence iscanceled by both boson and fermion loops.

t

t
ϕ

ht
−

2

hΛ
2
t

Even if SUSY,

(4π )

2

2

= 0

ϕ

ht2
1

1
(4π )

+ ϕ

ϕ

ht

ht2 Λ 2

Exact SUSY

2
⎛
⎞
Λ
2
2 2
δ mϕ ∼
h mt ln ⎜⎜ 2 ⎟⎟
2 t
(4π )
⎝ mt ⎠

1

)

∼

2W
M
(
O

∼

.
.
.

∼

2b
m

2t
m

We don’t need a fine tuning whenSUSY GUTThe coupling constants
are unified at

MX ≈ 10 GeV
16

A lot of newparticles ,which do not obey
the asymptotic free, appearatμ ≥ 102 GeVMartin, ”A Supersymmetry Primer”

MSSM• Minimal extension of Standard Model tosupersymmetry including two Higgs doublets

WMSSM = −uyu QH u + dyd QH d + eye LH d
dyd QH u* because of holomorphism in super pot.
⎛ hu+ ⎞
Hu = ⎜ 0 ⎟⎝ hu ⎠⎛ hd0 ⎞
Hd = ⎜ − ⎟⎝ hd ⎠• 105 masses, phases and mixing angles!!!

CMSSM
Constrained MSSM
Simplified into only five parameters from 105①

Common scalar mass at GUT scale: m0②

Unified gaugino (fermion) mass at GUT scale: m1/2③

Ratio of Higgs vacuum expectation values:④

Higgs/higgsino mass parameter (or its signature): μ⑤tri-linear coupling A0

tan β ≡

H u0
H d0

Super particles in CMSSM

stop
stau

sneutrinobino, wino, higgsinos

Martin, ”A Supersymmetry Primer”

Running of Renormalization Group (RG)
Equation in CMSSM

Negative Higgs mass term

Martin, ”A Supersymmetry Primer”

Mass spectrum in CMSSM

stop
sneutrino
stauneutralino
Martin, ”A Supersymmetry Primer”

Lightest SUSY particle (LSP)• R-parity conservationi)Decayτ → χ +τ(-1)(-1)× (+1)ii) Pair annihilation/production

f + f ↔χ+χ(+1) ×(+1)(-1)× (-1)

Thermal freezeout
Boltzmann equation

3Hnχ ∼σ v frezeout
TFreezeout ∼ mχ / 30

⎛
⎞
σv
⎜
⎟
2
Ω χ h ∼ 0.1⎜
2 ⎟
0.1
⎜
⎟
TeV ⎠
⎝

(

)

Ωχ does not depend on mχPredicting TeV Physics!!!

Kolb & Turner

σv = 3 × 10 −26cm 3 / s

LSP (LOSP) in CMSSM
Neutralino or Scalar tau lepton (Stau) is the Lightest Ordinary SUSY
Particle (LOSP)ΩLOSP= Ωobs

χ LOSPχ LOSP
τ

P
S
O
L

τ

P
S
O
L

ΩLOSP= Ωobs

Ellis,Olive,Santoso,Spanos(03)Supergravitiy (SUGRA)• Local theory of SUSY
(predicting gravitino)• Models of supersymmetry breaking(gravitino mass production by eating goldstino
which appears in spontaneous symmetry
breaking)• Including general relativity(Unifying space-time symmetry with local
SUSY transformation)SUSY Breaking Models
Gravity mediated SUSY breaking model
Observable sector

Only through gravity

quark, squark, …

Hidden sector

SUSY

F ~ 1020 −21 GeV 2

Masses of squarks and sleptons

mq , m = F / Mpl = 102 − 103 GeV(F = 1020 − 1021 GeV)

Gravitino mass

m3/ 2 = F / Mpl = 102 − 103 GeV

SUSY Breaking Models II
Gauge-mediated SUSY breaking model
Observable sector

SUSY breaking sector

quark, squark, …

SUSY

Gauge interaction

Messenger
sectorGauge interaction

m3/ 2 ~ F / Mp < 10GeVLightest SUSY particle (LSP) may be necessarily the gravitino

Signature of SUSY particles relatedwith Astrophysics and Cosmology• Direct detection• Indirect detection• Big-bang nucleosynthesis (BBN)• Cosmic Microwave Background (CMB)• Diffused gamma-ray backgroundDirect detection of LSP (LOSP) in
CMSSM
Annual modulation

s
/
m
k
0
3
n
u
s
e
h
t
d
n
u
o
r
a

g
n
i
v
o
m

June

s
/
m
k
0
2
2

χ
χ

χ

χ

χ
DecemberGelmini, arXiv:0810.3733v1

Indirect detection of LSP (LOSP)
Annihilation signals of neutralino at Galaxy Center, theSun, near solar system, etc…
Quite a lot of groups have contributed this topicχχ → WW , ZZ , Z γ , 2γ , e e
W , Z → broad spectrum of γ , e + e − , p p+ −Or gravitino/sneutrino decay with R-parity violation
Ibarra, Tran (08), Ishiwata, Matsumoto, Moroi (08), Chen, Takahashi (08)Or hidden gauge boson decay with kinetic mixing
Chen, Takahashi, Yanagida (08)

•
•
•
•
•

Gamma-ray from a point source
Anti-proton
Positron
511 keV line gamma
Neutrinos••••

Synchrotron radio
WMAP HAZE component
Nucleosynthesis
etc…

Positron Excess(PAMELA satellite reported)

Adriani et al, arXiv:0810.4995v1 [astro-ph]Electron and positron flux by ATIC2

Chang et al (08)

Positron Excess Hisano, Kawasaki, Kohri, Nakayama (08)Diffusion model

Flux
Steady-state solution (Hisano etal, ’06)
K(E) and b(E) are taken from (Baltz-Edsjo ’99)
Propagating within a few kpc, normalized to fit B/C, Boost
Factor (BF) considered for clumpy distributed DM.

rpropagation ∼ EK (E ) / b (E ) ∼ 0.7kpc(E / GeV) −0.17

Positron excess
in DM annihilation
Hisano, Kawasaki,
Kohri, Moroi, Nakayama in prep

Diffusion model
Fitted to B/C ratio

σv ∼ 10 −24 − 10 −23cm 3 / sElectron/positron cutoff
in DM annihilation
Hisano, Kawasaki,
Kohri, Moroi, Nakayama in prep

Diffusion model
Fitted to B/C ratio

σv ∼ 10 −24 − 10 −23cm 3 / s

Anti-proton flux

(PAMELA satellite reported)

Adriani et al, arXiv:0810.4994v1 [astro-ph]Consistent with secondary production of pp
or Leptonic DM ? by Chen-Takahashi (08)Gamma-ray anomaly at Galactic Center(EGRET satellite reported)

Consistent with secondary production of pp

Hunter et al (97)Gamma-ray signal in wino DM annihilation
Hisano, Kawasaki, Kohri, Nakayama, arXiv:0810.1892 [hep-ph]Gamma-ray flux

Averaged overProfile°°−5 < < 5−2° < b < 2°

Navarro-Frank-White (NFW): cusp structure

Isothermal (iso): core structureρ ∝ r − p ( p = 1 − 1.5)

ρ ∝ 1/[1 + (r / r0 )q ] (q = 2)

Gamma-ray signal in wino DM annihilation
Hisano, Kawasaki, Kohri, Nakayama, arXiv:0810.1892 [hep-ph]Fermi Sensitivity−5° < < 5°
−2 ° < b < 2 °H.E.S.S.

Gamma-ray signal in DM annihilation
Hisano, Kawasaki, Kohri, Moroi, Nakayama in prep

Neutrinos from galactic center expectedby PAMELA/ATIC2

Hisano, Kawasaki, Kohri, Nakayama (08)• Detecting up-going muons in
Kamioka• Annihilation (upper panel)and decay (lower panel)• Direct-neutrino emission
modes with NFW are
excludedBig-Bang Nucleosynthesis (BBN)
Very strong cosmological tools to study long-lived
particles with lifetime of 0.01 sec – 1012 sec
Theoretical predictions are constrained byobservational D, 3He, 4He, 6Li and 7Li
abundances with their conservatively-large
errors.

Lithium Problem
If we adopted smaller systematic
errors for observational data of 6Li
and 7Li , the BBN theory does notagree with observation of Li
abundances.

SBBN(4-5)×10-10
5×10-5(≡ nB / nγ )Lithium 7

a factor of two or threesmaller
T > !!!
5700 K ( ∝ M ), [Fe/H ] < -2
zObserved metal poor halo stars in Pop II

zAbundance does not depend on metalicity for“Spite’s plateau”

effzExpected that there is little depletion in stars.

7−10
Li / H = 1.26+−0.32
×
10
(1σ )
0.21

log ( 7 Li / H ) = −9.90 ± 0.09 (1σ )Ryan et al.(2000)
Bonifacio et al.(2006)

Lemoine et al., 1997

Lithium 6

Asplund et al.(2006)

zObserved in metal poor halo stars in Pop II
z6Li plateau?
6

Li / Li = 0.022 − 0.090

77Li / H ≈ (1.1 − 1.5) × 10

−10still disagrees with SBBN
Astrophysically, factor-of-two depletion of Li7 needs afactor of O(10) Li6 depletion (Pinsonneault et al ’02)
We need more primordial Li6?

Doppler broadening
Cold ISM

7Li

6Li

Knauth, Federman,
Lambert (2006)

LP815-43
Asplund et al.(2006)

7Li+6Li

Astrophysical uncertainties in Li7• Diffusion and convection
Korn et al (2006)

Li7

Destruction of Li7 in innerzone of stars
There is a increasing trendof both Iron and Li7 as afunction of TeffAstrophysical uncertainties in Li6
Cayrel, Steffen, Bonifacio, Ludwig and Caffau (2008)• Asymmetries of the absorption line mimicked byconvective motionMy attitude towards Li problem
It might be premature to accept that theseobservational values are purely primordial• Adding large systematic errors by hand andconstraining (non-)standard cosmologicalscenarios• Inventing a new cosmological/particle-physics
model to solve Li problem

Constraints on long-lived SUSY
particles from BBN• We add large systematic errors into
observational Li7 and Li6 abundacnes
log10 ( 7Li/H ) = −9.90 ± 0.09 ( ±0.35)syst.
Melendez,Ramirez(2004)

Li/ Li < 0.046 ± 0.022 ( ±0.106)sys

6

7Asplund et al(2006)

Massive particle decaying during/after BBN
epoch produces high energy photons,
hadrons, and neutrinos
Destruction/production/dilution of light elements
Severer constraints on the number density
Sato and Kobayashi (1977), Lindley (1984,1985), Khlopov and Linde (1984)
Ellis, Kim, Nanopoulos, (1984); Ellis, Nanopoulos, Sarkar (1985)
Kawasaki and Sato (1987)
Reno and Seckel (1988), Dimopoulos, Esmailzadeh, Hall, Starkman (1988)
Kawasaki, Moroi (1994), Sigl et al (95), Holtmann et al (97)
Jedamzik (2000), Kawasaki, Kohri, Moroi (2001), Kohri(2001), Cyburt, Ellis,
Fields, Olive (2003)
Kawasaki, Kohri, Moroi(04), Jedamzik (06)Radiative decay modex

D+p+n
He3/D >~ O(1)

Hadronic decay modex

Reno, Seckel (1988)
S. Dimopoulos et al.(1989)

Two hadron jets with

E jet = mX /3

Bh ≈ α / 4π ≈ 10−3x

One hadron jet with

E jet = mX /2

Bh = 1

（I) Early stage of BBN (T > 0.1MeV)
Reno and Seckel (1988) Kohri (2001)

Extraordinary inter-conversion reactions between n and pcf)

n +π + → p +π 0p +π − → n +π 0

weakstrongΓn ↔ p = Γ n ↔ p + Γ n ↔ p

Hadron induced
exchangeΓn ↔ p ↑ ⇒ n / p ↑Even after freeze-out of n/p in SBBN

More He4, D, Li7 …

(II) Late stage of BBN (T < 0.1MeV)
Hadronic showers and “Hadro-dissociation”

En= Ef(p)

S. Dimopoulos et al. (1988)
Kawasaki, Kohri, Moroi (2004)

Non-thermal Li, Be Production byenergetic nucleons or photons
dimopoulos et al (1989)
Jedamzik (2000)
3
⎧
He+X
4
3
N (or γ ) + He → ⎨
T,
He
+
X
T
⎩

He

4

N (or γ ) + He → He +X
4

4

*

He

4

Energy loss

① T(He3) – He4 collision
T + 4He → 6Li + n[8.4 MeV]

He + 4He → 6Li + p[7.0 MeV]3② He4 – He4 collision
He + 4He → 6Li, 7Li, 7Be + ...

4

Massive particle X
Upper bounds on mx Yx in both photodissociationand "hadrodissociation" scenario

Yx ≡ nx / s

Kawasaki, Kohri, Moroi (04)Mildobservational
upper boundMildobservational
upper boundNeutralino (bino) LSP and gravitino“NLSP”

Upper bound on reheating temperature
Kawasaki, Kohri, Moroi, Yotusyanagi (08)TR ≈ 109 GeV (Y3/ 2 /10 −12 )τ ∼ m pl2 / m33/ 2

Yx ≡ nx / s

Neutralino (bino) NLSP and gravitino LSPGravitino LSP and thermally porduced
neutralino (Bino) “NLSP” scenario
Feng, Su, and Takayama (03)Lifetimeτ ∼ m m pl / mNLSP
2
3/2

2

Relic abundancemB = 100GeV

5

Steffen (06)Kawasaki, Kohri, Moroi, Yotsuyanagi (08)No allowed region for
DM density

Sneutrino NLSP and gravitino LSP
scenario

Stable (left-handed) sneutrino was excluded by
the direct detection experiments because of its
large cross section directly-coupled with W/Zbosons.
(left-handed) sneutrino should be unstable

Gravitino LSP and thermally porduced
sneutrino NLSP scenario

Kawasaki, Kohri, Moroi, Yotsuyanagi (08)Relic abundance

Ellis, Olive, Santoso (08)mν = 300GeV

No allowed region for DM density with 100GeV sneutrinos

Stau NLSP and gravitino LSP scenario
Stable stau with weak-scale mass ( <100TeV)
was excluded by the experiments of ocean
water
NLSP stau should be unstable
Bound-state effect (see next)

CHArged Massive Particle (CHAMP)
Kohri and Takayama, hep-ph/0605243
See also literature, Cahn-Glashow (‘81)
Candidates of long-lived CHAMP in modern cosmology
stau, stop …
N+“CHAMP recombination” with light elemcts
Tc~ E bin/40 ~ 10keV
CHAMP(Ebin ~ α2 mi ~ 100keV )See also the standard recombination between electron and, (T ~ E /40 ~ 0.1eV, E ~ α m ~ 13.6eV ) )proton

c

bin

bin

2

e

CHAMP captured-nuclei, e.g., (C,4He) changes thenuclear reaction rates dramatically in BBN

Pospelov’s effectPospelov (2006),hep-ph/0605215• CHAMP bound state with 4He enhances
the rateD + ( He,C ) → Li + C
4

−

6

−

• Enhancement of cross section~ (λγ / aBohr ) ~ (30) ~ 10
5

5

7 −8

Confirmed by Hamaguchi etal (07), hep-ph/0702274

Stau NLSP and gravitino LSP
Scenario in gauge mediation
Kawasaki, Kohri, Moroi PLB 649 (07) 436

Relic abundance

Lifetime

τ>103secmτ = 100GeV

Lifetime

τ>103sec

Stau NLSP and axino/flatino LSP in
DFSZ axion models in Gravity Mediation

Chun, Kim, Kohri, and Lyth (08)Decaying “flatons”
reheats the universe andproduce staus
TR ~ O(10) GeV
Contrary to gravitino LSP
models, lifetime of stau is very
short due to milder suppression(∝Fa-2 ) and many couplings.

10 −8 sec < τ τ

10 −2 sec

No BBN Catalysis
Stau can be found in LHC!!!

Lifetime of stau NLSP decaying into
axino LSP
Chun, Kim, Kohri and Lyth (08)Can we distinguish gravitino fromaxino in LHC?
Brandenburg, Covi, Hamaguchi, Roszkowski, Steffen (05)

Large Hadron Collider (LHC)

10m~10-7sec

ATLAS detector in CERN, Geneva, SwitzerlandPlace another stopper near ATLAS or
CMS to stop long-lived charged SUSY
particles (even for cτ > 10 m)• 5 m Iron wall Hamaguchi, Kuno, Nakaya, and Nojiri (04)
• Water tankFeng and Smith (04)• Surrounded rock
De Roek, Ellis, Gianotti, Mootgat, Olive and Pape (05)Residual annihilation of DM even ataround BBN epoch• To fit the PAMELA and ATIC2 positron
signals and EGRET gamma-ray anomaly,σv ∼ 10 −24 − 10 −23cm 3 / s• At least it must emit charged leptons
Electromagnetic cascade shower is induced• It might also emit hadrons
Hadronic cascade shower is inducedHadron emission by residual annihilationin BBN epoch
Hisano et al in preparation

Charged-lepton (e+e-) emission by
residual annihilation in BBN epoch
Hisano et al in preparation

Solving Li problem in new particle
physics models• We do not adopt systematic uncertainties ofobservational Li7 and Li6 abundances

Can long-lived particles solve the Li problem?
• Neutralino LSP and stau NLSP with small
mass deference (<100 MeV)
Bird,Koopmans,Pospelov(07), Jittoh etal (07,08)• Residual annihilation of wino-like neutralino
LSP with more massive gravitino
Hisano et al (08)• Stop NLSP and gravitino LSP scenario
Kohri and Santoso (08)Reduction of 7Li and production
Jedamzik (04) , Cumberbatch et al (08)of 6Li• Copious neutrons and tritiums are produced in
hadronic shower process with decay/annihilation
Jedazmik (‘04)• Reducing Be7 throughBe(n,p) Li(p, He) He

7

7

4

4

( 7Li is produced later by 7Be + e - → 7Li + ν e )• Tritium scatters off the background He4 andDimopoulos et al (‘89)
produces Li6

T+4He → Li+n6

Stop NLSP and gravitino LSP
Kohri and Santoso (08)• Stop can be NLSP in Non-universal Higgs masses(NUHM)• Stop is confined into “messino” after QCD phasetransition• Second annihilation of stop occurs just after QCD
phase transition through strong interaction• Stop number density is highly suppressed, but it isappropriate to solve the Li problem

mt nt / s ∼ 10

−14

GeV − 10−13

GeVStop NLSP and gravitino LSP

Kohri and Santoso arXiv:0811.1119v1 [hep-ph]Residual annihilation of wino
Hisano, Kawasaki, Kohri, Nakayama(08)LSP• Non-thermal production of wino LSP bydecaying massive such as gravitinos (> O(10)TeV)

ψμ →w +w

• Annihilating even after wino’s freeze-out timewith its larger annihilation rate than bino’s
σv >> 3 × 10 −26cm 3 / s

WW → WW

Even during/after BBN epoch!!!

Residual annihilation of wino-like LSP
Hisano, Kawasaki, Kohri, Nakayama(08)Thermal(bino) DM
We need nonthermal wino production by gravitino decay

Conclusion• Direct and indirect detections of DM will become more
attractive in near future to get information on SUSY andSUGRA• BBN is a strong tool to investigate the long-lived SUSY particles,
such as gravitino, neutralino, stau, stop, or axino• In neutralino LSP and unstable gravitino scenario in gravity
mediated SUSY breaking models, the constraint on reheating
temperature after primordial inflation is very stringent,TR ≤ 3 × 105 GeV − 107 GeV(for m3/ 2 = 100 GeV − 1TeV)• In gauge mediation, thermal-relic NLSP fails to produce DM
gravitino density for natural scales of NLSP masses (100GeV –1TeV) . We need thermal or nonthermal production of LSP
gravitino by the decay of Inflaton, moduli etc.
See Moroi, Murayama, Yamaguchi (93) for thermal production, and Endo,
Takahashi, Yanagida (07) for non-thermal production of LSP gravitino

Another ideas

Hooper, Blasi, Serpico (08)• positrons produced in pulsars