Charged SUSY particles and their effects on cosmology

Physics Department, Lancaster University Physics Department, Lancaster University

Kawasaki, Kohri, Moroi, PRD71 (2005) 083502

（郡 和範）Kazunori KohriKazunori Kohri

Kawasaki, Kohri, Moroi, PLB625 (2005) 7

Kohri, Moroi, Yotsuyanagi, PRD73 (2006) 123511

Kanzaki et al, hep-ph/0609246

Kohri and Takayama, hep-ph/0605243

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= ≈

Non-thermal Li6 ProductionDimopoulos et al (1989)

Jedamzik (2000)

Kawasaki,Kohri,Moroi (2001)

γ⎧ +

→ ⎨+⎩

34 HeHe+

np T

→4 6T + He Li+ [8.4 MeV]n→3 4 6 He+ He Li+ [7.0 MeV]p

Coulomb energy loss by background electrons

i. He3 (T) production

ii. Li6 production

παβΛ

= Λ2 24 , ~ (1)e

e

Z ndE Odx m

3T, He 4He

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)

↔ ↔↔Γ = Γ + Γstrongweakn p n pn p

Extraordinary interExtraordinary inter--conversion reactions between n and pconversion reactions between n and p

Hadron induced exchange

↔Γ ↑ ⇒ ↑ /n p n pEven after freeze-out of n/p in SBBN

More He4, D, Li7 …

cf) 0n pπ π++ → + 0p nπ π−+ → +

（（I) Early stage of BBN (before/during BBN)I) Early stage of BBN (before/during BBN)Reno and Seckel (1988) Kohri (2001)

(II) Late stage of BBNHadronic showers and “Hadro-dissociation”

S. Dimopoulos et al. (1988)

fE E=n (p)

Kawasaki, Kohri, Moroi (2004)

Jedamzik (2006)

Non-thermal Li, Be Production by energetic hadrons Dimopoulos et al (1989)

⎧→ ⎨

⎩

34 He+X

N + HeT + X

→4 6T + He Li + [8.4 MeV]n

→3 4 6 He + He Li + [7.0 MeV]p

→4 4 *N + He He +X

→4 4 6 7 7He + He Li, Li, Be + ...

3T, He4He

4He Energy loss

① T(He3) – He4 collision

② He4 – He4 collision

( )−= 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

Sneutrino NLSP, Gravitino LSP and inplication for Thermal Leptogenesis

Kanzaki, Kawasaki, Kohri, Moroi (2006)

Thermal-relic sneurinos can not produce sufficient DM Ω3/2

This region might be excluded in neutralino / stau

NLSP scenarios

μν ν ψ→ +

Feng, Su, Tankayama (04)

Steffen (06)

( )14~ 2 10 /100GeVY mν ν−×

Fujii, Ibe, Yanagida (04)

1()

Mm ν

>

High TR

Only reheating process can produce sufficient Gravitino DM Ω3/2h2～ 0.11

Lighter gravitino mass

larger gaugino mass (σ∝M12 )

Overproduction of Gravitinos for a fixed TR

Higher TR can be realized at

Larger gravitino mass

lighter gaugino mass

Ω3/2h2 ～ 0.11Different from neutralino / stau NLSP scenario !

Thermal Leptogensis (Fukugita and Yanagida (1986), Buchmuller, Bari,

Pluacher (05) ) does still work!

Solving Li7 problem in Hadronic decaySolving Li7 problem in Hadronic decay

severer 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!

-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)

6+ Li+Dα α →More Li6 can be also produced!

Kohri et al (2006)

CHArged Massive Particle (CHAMP) and Cosmology

Many candidates of long-lived CHAMP, e.g., scalar leptons (stau etc) as NLSPs, which eventually decays into DM (gravitino) and standard particles

More massive elements tend to capture CHAMP earlier because of larger binding energy of the bound states (Tcapture =Ebin/40 ~ 1-10 keV, Ebin ~α2 Z2

champ Z2nuc mnuc)

Note that ligher nuclei have been freezeout after T= Tcapture

CHAMP captured-nuclei change the nuclear reaction rates through the modifications of the Coulomb suppression factor and their kinematics.

Only Be7 and Li7 can be reduced without changing D, He3, andHe4 abundances

Kohri and Takayama, hep-ph/0605243

Cahn and Glashow (1981)

Binding energy Ebin ~ α2 Z2champ Z2

nuc mnuc

Time evolution of light elementsTime evolution of light elements

CHAMP (ChArged Massive Particle) and BBN

Charged particles may recombine with light elements to form bound states such as a hydrogen atom in the early

Universe for T < Ebin /40 (~ 1-10 keV)C-

Nucleus+

At least

Charge suppression

Kinetic energy modification into the order of binding energy Ebin = α2mnuc~O(0.1) – O(1) MeV (note that E~T in SBBN )

Pospelov’s Effect? - possible enhancement of cross sections in quadrupole -

Interesting!, but still some unclear points (lack of cross section data of He4(d,γ)Li6 at E < 0.1 MeV, etc…)

Pospelov (06)

Kohri and Takayama (06)

Kaplinghat and Rajaraman (06)

Cyburt, et at (06)

CHAMP BBN (CBBN) may solve Lithium problem? I

Short lifetime ( < 106 sec)• Only Be7 and Li7 captures CHAMP• Be7 (n,a)He4 and Li7(p,a)He4

are enhanced

Kohri and Takayama, hep-ph/0605243

However, the experimental data of the cross section for Be7 (n,a)He4is not sufficent at E = O(Ebin)

Here 10 times larger uncertainty in p-wave mode is assumed (see Serpico et al (04) [B-II case]

We need correct experimental data at E = Ebin

CHAMP BBN (CBBN) may solve Lithium problem? II

Long lifetime ( > 106 sec)Znuc =1 nuclei (proton, D, and T) are captured He4(d, g)Li6 and Be7(d, p a)He4are enhancecd

Kohri and Takayama, hep-ph/0605243

However, CHAMP may change its partner from p,D, T into more massive ones before nuclear reactions occur because

> nucBohra rShould we solve the three body problem?

Discussion and ConclusionDiscussion and Conclusion• The radiative and hadronic decay products destroy He4, by

which D,He3, Li6 are overproduced.

• The constraint on reheating temperature after primordial inflation becomes very stringent in Hadronic decay scenario of unstable gravitino.

• Hadronic-decay scenario may solve the Li problem

• Gravitino LSP, Sneutrino NLSP scenario agree with Thermal Leptogeneis

• CHAMP BBN is attractive (Kohri and Takayama ‘06, Cyburt etal‘06) or might be dangerous? (Pospelov ‘06).

5

3/2

7

(for 100 GeV a few T3 10 GeV 10 GeV

eV)R

mT

= −

≤ × −