Long-lived charged massive particle and the effect on cosmology

Physics Department, Lancaster University Physics Department, Lancaster University

Kawasaki, Kohri, Moroi, PRD71 (2005) 083502

（郡 和範）Kazunori KohriKazunori Kohri

Kohri, Takayama, PRD (2007) in press, hep-ph/0605243

Kawasaki, Kohri, Moroi, PLB 649 (2007) 436

Jittoh, Kohri, Sato etal, arXiv:0704.2914 [hep-ph]

Cumberbatch etal, arXiv:0708.0095 [astro-ph] Chun, Kim, Kohri and Lyth, in preparation

AbstractAbstract• The Standard Big Bang Nnucleosynthesis (SBBN)

approximately agrees with observations.

• We can use BBN as a probe to study the early universe

• In SUSY/SUGRA cosmology, reheating temperature after Inflation should be less than 106GeV, in order to solve the “gravitino problem.”

• We may solve the Lithium problems in SUSY/SUGRA cosmology models

• Dark matter (LSP) may be neutralinos, gravitinos, or axinos which are nonthermally produced by decays of long-lived NLSP (gravitino, sneutrino or stau)

Gravitino Problem

Gravitino is the superpartner of gravitonμψ

Fermion Boson

Introduction of SUSYIntroduction of SUSYSupersymmetry (SUSY)

Solving “Hierarchy Problem”

Realizing “Coupling constant unification in GUT”

quark squark

lepton slepton

gravitino graviton

photino photon

Spin 3/2

2 2 3SUSY3/2 / 10 10 GeVplm M M= = −

SUSY BreakingSUSY Breaking

Gravity mediated SUSY breaking model

Observable sector

quark, squark, …

Hidden sector

SUSY

= −10 11SUSY( 10 10 GeV)M

Only through gravity

Masses of squarks and sleptons

Gravitino mass

= = −2 2 3SUSY, / 10 10 GeVq plm m M M

SUSYM

3/2 10GeVm <

SUSY Breaking IISUSY Breaking IIGauge-mediated SUSY breaking model

(Dynamical SUSY brasking)Observable sector

quark, squark, …

SUSY breaking sector

SUSY

Messenger sector

Gauge interactionGauge interaction

Reviews of Long-Lived Massive particle (NLSP) in SUSY/SUGRA Cosmology

The interaction related with gravitions is highly suppressed

3/2 / plg m m∼2

NLSP LSP 3/23 23/2 pl

6 1

/

(1 10 sec)

g mm m

→

−

Γ

−

∼

∼

∼

3/2For 100GeV - 10TeVm ∼

Gravitino Decay and BBNGravitino Decay and BBN1. Gravitinos are unstable in Gravity Mediation SUSY

Radiative decay

Hadronic decay

τ ψ γ γ−

⎛ ⎞→ + = × ⎜ ⎟⎝ ⎠

38 3/2

3/2m( ) 4 10 sec

100 GeV

τ ψ−

⎛ ⎞→ + = × ⎜ ⎟⎝ ⎠

37 3/2

3/2m( ) 6 10 sec

100 GeVg g

1Bγ =

1 ( (1))hB B Oγ= ≈

Hadronic decayHadronic decay

=jet

One hadron jet with/2XE m

=jet

Two hadron jets with/3XE m

3/ 4 10hB α π −≈ ≈

1hB =

Reno, Seckel (1988)

S. Dimopoulos et al.(1989)

NLSP decays during/after BBN epoch producing high energy photons and hadrons

Destruction/Production of light elements

Severer constraints on the reheating temperature RT

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), Kawasaki, Kohri, Moroi (2001), Kohri(2001)

Jedamzik (2000), Cyburt, Ellis, Fields, Olive (2003)

Kawasaki, Kohri, Moroi (2004)

He4

D/H

Li7/H

Li6/H

He3/D

Observational Light Element Observational Light Element AbundancesAbundances

pY 0.2516 0.004= ±Peimbert,Lridiana, Peimbert(2007)

Izotov,Thuan, Stasinska (2007)

5D/H (2.82 0.26) 10−= ± ×

Melendez,Ramirez(2004)( )710 syst.log Li/H 9.63 0.06 ( 0.3)= − ± ±

O’Meara et al. (2006)

6 7Li/ Li 0.046 0.022 0.084< ± ± Asplund et al(2006)

3He/D 0.83 0.27< + Geiss and Gloeckler (2003)

Fukugita, Kawasaki (2006)

Constraints on massive particle XConstraints on massive particle X

τx x xC o n t o u r s o f l i g h t e l e m e n t s i n ( m Y , ) p l a n e i n " h a d r o d i s s o c i a t i o n " s c e n a r i o

XX

nYs

≡

Yield variable and reheating temperature

Lifetime and mass

γ

− ⎛ ⎞≡ = × ⎜ ⎟⎝ ⎠

113/23/2 101.1 10

10 GeVRn TY

n

τ ψ γ γ−

⎛ ⎞→ + = × ⎜ ⎟⎝ ⎠

38 3/2

3/2m( ) 4 10 sec

100 GeV

Relation among variablesRelation among variables

( )−= 9 123/210 GeV /10RT Y

Upper bound on reheating temperatureUpper bound on reheating temperatureKawasaki, Kohri, Moroi (2004)

τ −= × 5 1/33/2 3/2500GeV ( /4 10 sec)m

μψ → + =( ) 1hB g g

Lithium Problems

SBBN

( / )Bn nγ≡

7 -10SBBN( Li/H) =(4-5)×10

Li6/Li7～3.3×10-5

Lithium 7

Observed metal poor halo stars in Pop II

Abundance does not depend on metalicity for

Expected that there is little depletion in stars.eff 5700 K ( ), [Fe/ ] -2T M H> ∝ < “Spite’s plateau”

Lemoine et al., 1997

7 0.68 100.32Li / H 1.23 10+ −−= ×

Ryan et al.(2000)

a factor of two or three smaller !!!

Bonifacio et al.(2006)

Lithium 6Observed in metal poor halo stars in Pop II6Li plateau?

Asplund et al.(2006)

7 10Li / H (1.1 1.5) 10 −≈ − ×

6 7Li / Li 0.002 0.090= −

Astrophysically, factor-of-two depletion of Li7 needs a factor of O(10) Li6 depletion (Pinsonneault et al ’02)

We need more primordial Li6?

still disagrees with SBBN

Solving Li7 problem in Hadronic decay of neutral Solving Li7 problem in Hadronic decay of neutral particlesparticlesSeverer observations

7 -10SBBN( Li/H) =(4-5)×10

?

Neuron emission from hadronic shower

7 4Be ... 2 Hen+ → →

7 7( Be Li + )e γ−+ →

Li7 can be reduced! (Jedamzik)

-10WMAP(η=η =(6.1±0.6)×10 )

Kohri, Moroi, Yotsuyanagi (2005)

Jedamzik (04); Jedamzik etal (05)

10(2 4) 10 at 2η σ−= − ×

Ryan etal (‘00), Asplund etal (‘05)

3 4 6He+ He Li+p→More Li6 can be also produced!

Cumberbatch etal (2007)

NLSP might be Slepton? (stau or sneutrino)

LSP would be gravitino, or neuralino with small mass-difference

Neutralino NLSP would be excluded by BBN because of high hadronic branching ratio

Feng, Su, and Takayama (2003)

Steffen (2006)

Kanzaki, Kawasaki, Kohri, Moroi (2006)

CHArged Massive Particle (CHAMP)

Many candidates of long-lived CHAMPstau, …

More massive elements capture CHAMP earlier Tc~ E bin/40 ~ 10keV (Ebin ~ α2 mi ~ 100keV )

CHAMP captured-nuclei change the nuclear reaction rates

Kohri and Takayama, hep-ph/0605243

N+

CHAMP-

See also literature, Cahn-Glashow (‘81)

CHAMP BBN (CBBN) may solve Lithium problem?

Short lifetime ( < 103 sec)• Only Be7 and Li7 captures CHAMP• Be7 (n,a)He4 and Li7(p,a)He4

are enhanced

Long lifetime ( > 106 sec)• Z=1 elements, proton, D, and T are captured • He4(d, g)Li6 and Be7(d, p a)He4

are enhanced

However, the Bohr radius might betoo large to completely suppress thecoulomb field?

Kohri and Takayama, hep-ph/0605243

(See also, recent work by Jedamzik, arXiv:0707.2070)

(Kohri and Takayama, hep-ph/0605243)

Pospelov’s effect

• CHAMP bound state with 4He can enhance the rate

• Enhancement of cross section

4 6D ( He,C ) Li γ−+ → +

Pospelov (2006),hep-ph/0605215

5 5 8Bohr~ ( / ) ~ (30) ~ 10aγλ

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

BBN in stau NLSP and gravitino LSP Scenario in gauge mediation

Kawasaki, Kohri, Moroi PLB 649 (07) 436

See also, Jedamzik, arXiv:0707.2070

Difficulties in CBBN for long lifetime (> 1000 sec)

Stau NLSP and neutralino LSP Scenario in Gravity Mediation

Jittoh, Kohri, Sato etal, arXiv:0704.2914

00.1GeVm m mτ χδ = − <

Effectively Be7, Li7 are destroyed!!!

DM,obsΩ

NLSP

DM

See also Bird, Koopman and Pospelov (07)

No CBBN Catalysis

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

Chun, Kim, Kohri, and Lyth in preparation

Decaying flatons reheat universe and produce staus

TR ~ O(10) GeVContrary to gravitino LSP models, lifetime of stau is very short

ττ−210 sec

No CBBN Catalysis

Or lower reheating temperatures no longer produce staus

Note also the mechanism discussed in Dr. Kasuya’s today’s talk

ConclusionConclusion• The constraint on reheating temperature after

primordial inflation is very stringent in Hadronic decay scenario in gravity mediated SUSY breaking models.

• CHAMP BBN is attractive in stau NLSP scenario. Then DM should be a stable gravitino in gauge-mediated SUSY breaking models, or neutralino with small mass difference or axinos in gravity mediated SUSY breaking models.

−

−

≤

=

×

3/

5 7

2(for 103 10 GeV 10 G

0 GeV 10 VV

ee

T )RT

m