The Cosmic Lithium Anomalies:Signs of the Dark Universe ?

Karsten JEDAMZIK†

† LPTA, Montpellier

Karsten Jedamzik, Brighton, August ‘07 – p. 1

The 7Li Problem in standard BBN

1e-10

2e-10

3e-10

4e-10

5e-10

6e-10

7e-10

1 2 3 4 5 6 7 8 9 10

Li/H

"observed""predicted"

Ryan et al 00; Bonifacio & Molaro 97; Charbonnel & Primas 05; Boesgard et al 05, Melendez& Ramirez 04; Asplund et al 05; Bonifacio et al 03, Zhangf & Zhao 04

Burles et al 01; Cyburt et al 04; Coc et al 04; Cuoco et al 04

Karsten Jedamzik, Brighton, August ‘07 – p. 2

6Li at low metallicity: A surprise

Asplund, Lambert, Nissen, Primas, and Smith 05 (astro-ph/0510636)

Karsten Jedamzik, Brighton, August ‘07 – p. 3

6Li ,7Li Situation Summary

7Li observed factor 2 − 3 lower in old stars than produced inSBBN Astrophysical Solutions: Depletion in stars, Nuclear

cross sections, Stellar Atmospheres

Karsten Jedamzik, Brighton, August ‘07 – p. 4

6Li ,7Li Situation Summary

7Li observed factor 2 − 3 lower in old stars than produced inSBBN Astrophysical Solutions: Depletion in stars, Nuclear

cross sections, Stellar Atmospheres

6Li observed factor 1000 higher in old stars than produced inSBBN Astrophysical Solutions: Very early cosmic ray

population, solar flares, observational error

Karsten Jedamzik, Brighton, August ‘07 – p. 4

6Li and 7Li in cascade nucleosynthesis

n(4He,pn)3H(α, n)6Li at T ≈ 10 keVDimopolous et al 88, K.J. 00

7Be(n, p)7Li(p, α)4He at T ≈ 30 keVK.J. 04

Karsten Jedamzik, Brighton, August ‘07 – p. 5

Decaying neutral particles during BBN

0.1

1

100 1000

no bound states

Bh = 10-4

YX

τ (sec)

7Li7Li + 6Li

6Li

K.J. Phys. Rev. D 70 063524 (2004); (astro-ph/0402344)

Karsten Jedamzik, Brighton, August ‘07 – p. 6

Charged relic - nuclei bound states during/after BBN

Pospelov 06 Kohri & Takayama 06, Kaplinghat & Rajaraman 06, Cyburt et al 06, Hamaguchiet al. 07, Bird, Koopmans, & Pospelov 07, Kawasaki et al. 07, Takayama 07, Jittoh et al. 07

7Be + X−

→ (7Be − X−) + γ, 4He + X−

→ (4HeX−) + γ, etc.

reduction of Coulomb barrier → enhancement ofnuclear reactions

radiative capture reactions, e.g. 2H +4He→6Li +γ arereplaced by 2H +(4HeX−) →6Li +X−when 4He is inbound state → strong factor enhancement of rate

shifting binding energies may make reaction proceedingover nuclear resonances at thermal energies available,i.e. 7Be-X− + p →

8B-X− + γ

Karsten Jedamzik, Brighton, August ‘07 – p. 7

Decaying charged particles during BBN

0.1

1

100 1000

bound states

Bh = 10-4

YX

τ (sec)

7Li7Li + 6Li

6Li

Karsten Jedamzik, Brighton, August ‘07 – p. 8

The Cosmic Lithium Problems solved by Gravitino Warm DM

mSUGRA with gravitino LSP:

1/2m210 310

0m

10

210

310

τ-410 -310 -210 -110 1 10 210 310 410 510 610 710 810 910

2 hG

Ω

-610

-510

-410

-310

-210

-110

1

10

K.J., Choi, Roszkowski, Ruiz de Austri 05, Bailly, K.J., Moultaka 07

Karsten Jedamzik, Brighton, August ‘07 – p. 9

Further solutions to the 6Li and 7Li problems ?

Presence of X− leads to significant production of 6Li

Pospelov 06

Karsten Jedamzik, Brighton, August ‘07 – p. 10

Further solutions to the 6Li and 7Li problems ?

Presence of X− leads to significant production of 6Li

Pospelov 06

at T<∼

1 keV significant fraction of p are in bound states→ absence of Coulomb barrier

reactions (pX−)+6Li→ X−+4He+3He and(pX−)+7Be→ 8B + X−may destroy priorly synthesized 6Li

and 7Li Jedamzik 07

importance of charge exchange reaction(pX−)+4He→ p+4HeX−

Karsten Jedamzik, Brighton, August ‘07 – p. 10

6Li and 7Li with bound states at late times

1e-14

1e-13

1e-12

1e-11

1e-10

1e-09

1e-08

0.001 0.01 0.1 1 10 100

T (keV)

ni/nH

Karsten Jedamzik, Brighton, August ‘07 – p. 11

Solutions to the 6Li and 7Li problems due to bound states

1e-06

1e-05

1e-04

0.001

0.01

0.1

1000 10000 100000 1e+06 1e+07 1e+08 1e+09 1e+10 1e+11 1e+12

sigex = 10-18cm3/s

Yx

1e-06

1e-05

1e-04

0.001

0.01

0.1

1000 10000 100000 1e+06 1e+07 1e+08 1e+09 1e+10 1e+11 1e+12

sigex = 10-16cm3/s

Yx

K.Jedamzik (astro-ph/07072070)

Karsten Jedamzik, Brighton, August ‘07 – p. 12

Conclusions

standard BBN predicts factor 2 − 3 more 7Li thanobserved at low [Z]

6Li is observed in abundance at low metallicity,inconsistent with cosmic ray nucleosynthesis

the 6Li and/or 7Li problems mat be explained by decaying(annihilating) particles during BBN

if the decaying particle is charged (e.g.. τ ) 6Li may be firstsynthesized in abundance, and subsequently be againdestroyed at T<

∼1 keV along with 7Li

may be realised by gravitino dark matter in the CMSSM

Karsten Jedamzik, Brighton, August ‘07 – p. 13

6Li due to residual dark matter annihilation during BBN

10-27

10-26

10-25

10-24

10 100

Mx (GeV)

K.J. Phys. Rev. D 70 083510 (2004) (astro-ph/0405583)

Karsten Jedamzik, Brighton, August ‘07 – p. 14