Dark Matter

Expect Unexpected outside LHC

Jingsheng Li

Introduction

SM is confirmed precisely?

NO! Dark Matter is OUT THERE!!

SC=SM+more ∟(New Phy=ptc+int) +unexpected ∟astrophy effect? ∟ modify gravity?

Outline

Standard CosmologyEvidence for Dark MatterRelic DensityCandidatesDark Matter Detection

Standard Cosmology Smooth Universe

Friedman Eqn

Content ( w=/P, )

baryon w=0 radiation w=1/3 c.d.m. w=0 c.c. w=-1

28

3

a G

a

2 2 2{ 1, , , }g diag a a a

4( 3 )

3

a GP

a

3~ a

4~ a

3~ a

0~ a

/i i cr

20.0223 0.04b h 54.94 10 , 0.68

0.23CDM 0.74

1total

A Brief History of Universe

Properties of DM

Dark (rotation curve, gra. lensing) Cold (Structure formation)Weakly Interacting (rotation curve, Bullet Cluster)

b/m=1/6 (BBN, CMB, Bullet Cluster 1E0657-558)

Evolution of CDM Boltzmann Eqn (1+23+4)

Note:

Eq (T>m), freeze out (T<m)

33 1 3 4 1 2

1 23 4 1 2

( ) eq eqeq eq eq eq

d n a n n n na n n

dt n n n n

2 / eq eqi in H a a n n

3

3/2 /( )eq

m T

T m Tn

mT e m T

Relic Density

XX ll . .. .X f of on H

3 3

. .. .

. . . .

f oX X X o oo X o X f o X

f o f o

HT Tm n m n m

T T

32 3. .

. . . .

f o o X oX

Pl f o f o Pl

T T m Tm

M T T M

10 22 10

X

GeVh

29 2

2~ 0.1 ~ 10 ~ 0.1

SUSYW

GeVm

Lee-Weinberg Bound

Anti-baryon 45GeV L Scalar DM Higgs exchange, even weaker,

expect for Boehm, Fayet (N=2)

33 2 2( )

( )eq

d naa n n

dt change variable 2 2( )

[ ( ) ( )]eq

du xB u x u x

dx

0.51 0.54 0.542 2/ 3.7 3.7 10X X Mm h GeV h GeV GeV

F N

2 2 / 2F XG m F

2 2 2/ F Nm G mF 2 116 10B Bh

2 3100, 100, 10h N F

Lee-Weinberg is good for >GeV range

Candidate VS TestGra

LensingLee-Weinberg

+Z widthDirect Search

PAMELA/ATIC

MACHOs XAnti-Baryon X

SM L X

MSSM X

Neutralino X?

Gravitino -- ?

Axion -- ?

L

UED w/ KK-parity, LH w/ T-parity, Techni Baryon, monopole, R….

SUSY WIMP SUSY w/ R-parity provides LSP Spctrum depends on Mediation Scheme

Hidden Sector GMSB: gravitino as LSP, cosmo constraint:

NLSP decay, BBN and CMB constraints

Gravity Mediated , decay, BBN constraint Neutralino as LSP: In Lee-Weinberg bound2 2 2/F WG m M , ~XM m TeV

3/2 ~ / Plm F MF2 23/2 100m eV

3/2 ~m TeV

Neutralino Decay channels

univ~10Gyr, set upper bound for Mh2<0.3,

lower bound for , upper bound for mint.

Cosmology set upper bound on superpartner, good for LHC?

2 29 2

40.3 10 200f

ff

mGeV m m GeV

m

Axion (non-thermal CDM) PQ SSBAxion PQ EB

Coupling to Nucleon Red Giant emission bound SN1987A bound

Oscillation energy Critical density bound

Search:

~ /a aom m f f

~ /A N ag N m f

2

7 220010 a i

aPl i a

f MeV Ah

M T f

112 10af GeV

1210af GeV

/ aia fia af e f e

1010af GeV

ag aE B 101.16 10 for 0.02a ag m eV

Detection

MET

Direct Detection

Indirect Detection

Direct Detection

Type Scintillator Cryogenic Crystal

Noble Liquid

matterial NaI, CsI Ge, Si Ar, Xe

Pro Normal T Distinguish e / N New tech, potential

Con Background Low T, $

Exp DAMA CDMS XENON

Result Solar modulation

Indirect Detection

Annihilation at Center of Sun Galaxy Center Haloin to e+

detected by AMANDA, IceCube

GLAST, HESS, INTEGRAL

AMS, HEAT, PAMELA, ATIC

Result 511KeV from bulge

excess

Result from indirect detection e+ excess beyond prediction

10 GeV ~ 100GeV (PAMELA), e+e- excess upto TeV (ATIC)

ATIC: sharp falling @ 600GeVno astrophy explaination

SUSY needs 10TeV for PAMELA

No p- excess

Usual Neutralino can’t explain

Very large <v>, conflicts with required relic density.

Solution?

New interaction to annihilate Sommerfeld enhancement (Arkani-Hamed)

Breit-Wigner enhancement (Murayama)

Nonthermal production (Kumar)

DM decay