How to best reconcile Big Bang Nucleosynthesis with Li abundance determinations? Exotic BBN

Transcription

1 How to best reconcile Big Bang Nucleosynthesis with Li abundance determinations? Exotic BBN

2 Ryan et al.

3 Possible sources for the discrepancy Nuclear Rates - Restricted by solar neutrino flux Discussed by Coc - Role of resonances Stellar Depletion Discussed by Richard, Korn, Lind Stellar parameters dli dlng =.09.5 dli dt = K Discussed by Ryan

4 Possible sources for the discrepancy Stellar Depletion Discussed by Richard, Korn, Lind Stellar parameters dli dlng =.09.5 Particle Decays dli dt = K Discussed by Ryan

5 Limits on Unstable particles due to Electromagnetic/Hadronic Production and Destruction of Nuclei 3 free parameters ζ X = n X m X /nγ = m X Y X η, m X, and τ X Start with non-thermal injection spectrum (Pythia) Evolve element abundances including thermal (BBN) and non-thermal processes.

6 E.g., Gravitino decay Cyburt, Ellis, Fields, Luo, Olive, Spanos eg! f f, e G! + W (H ), e G! 0i (Z), e G! 0i H 0 i e G! gg. plus relevant 3-body decays

7 D/H 3e-05 7 Li/H 1e Li/ Li 0.1 1e τ (sec) Jedamzik Kawasaki, Kohri, Moroi

8 x x x x x Based on m 1/2 = 300 GeV, tan β =10 ; B h ~ 0.2

9 CMSSM 3000 M in = M GUT, tan = 10, µ > M in = M GUT, tan = 55, µ > 0 m 0 (GeV) 2000 m 0 (GeV) m 1/2 (GeV) m 1/2 (GeV) EOSS

10 Gravitino Decays and Li m 3/2 = 250 GeV m 3/2 = 250 GeV = 500 GeV = 750 GeV = 500 GeV = 750 GeV = 1000 GeV = 1000 GeV = 5000 GeV = 5000 GeV Cyburt, Ellis, Fields, Luo, Olive, Spanos

11 3 x x x x co-annihilation strip, tan β =10 ; m 3/2 = 250 GeV

12 3 x x x x co-annihilation strip, tan β =10 ; m 3/2 = 1000 GeV

13 x x x x x Benchmark point C, tan β =10 ; m 1/2 = 400 GeV

14 Uncertainties There are only a few non-thermal rates which affect the result p 4 He np 3 He 20% p 4 He ddp 40% dp 4 He dnpp Liγ 40% t 4 He 6 Lin 20% 3 He n 4 He dt 6 Lip 20% n 4 He npt 20% n 4 He ddn 40% n 4 He dnnp 40% p 4 He ppt 20% n 4 He nn 3 He 20% Log! 3/ / (n 4 He npt), Li/H m 3/2 (TeV)

15 How well can you do χ 2 ( ) ( 2 Yp D H ) Li H i s 2 i, SBBN: χ 2 = field stars SBBN: χ 2 = GC stars* -8 Point C * -9 is probably beyond the reach of present-day interferometers. NGC 6397 appears to have a higher Li content than field stars of the same metallicity. This needs to be confirmed by a homogeneous analysis of field stars, with the same models and methods. This may or may not be related to the fact that this cluster is nitrogen rich, compared to field stars of the same metallicity (Pasquini et al. 2008). Log 3/ * from Gonzales Hernandez et al m 3/2 (GeV)

16 m 3/2 [GeV] Log 10 (ζ 3/2 /[GeV]) Y p D/H ( 10 5 ) 7 Li/H ( ) s 2 i χ 2 BBN C E L M C M C C Point C -8 Point C -9-9 Log 3/ Log 3/ increased uncertainty in D/H GC value for Li m 3/2 (GeV) m 3/2 (GeV)

17 General feature of fixing Li: Increased D/H 4.5x x x10-10 Point C 4x10-10 Point E 3.5x x Li/H 3x Li/H 3x x x x x x x x x x x10-5 3x10-5 4x10-5 5x10-5 6x10-5 7x10-5 8x10-5 9x x x10-5 3x10-5 4x10-5 5x10-5 6x10-5 7x10-5 8x10-5 9x D/H D/H Cyburt, Ellis, Fields, Luo, Olive, Spanos Olive, Petitjean, Vangioni, Silk

18 Evolution of D, Li With post BBN processing of Li, D/H reproduces upper end of absorption data - dispersion due to in situ chemical destruction Olive, Petitjean, Vangioni, Silk

19 Effects of Bound States In SUSY models with a ~ τ NLSP, bound states form between 4 He and ~ τ The 4 He (D, γ) 6 Li reaction is normally highly suppressed (production of low energy γ) Bound state reaction is not suppressed D γ D 6 Li 4 He 6 Li 4 ( HeX ) X Pospelov

20 2000 m 3/2 = 100 GeV, tan β = 10, µ > m 3/2 = 100 GeV, tan β = 10, µ > 0 7 Li = He/D = 1 7 Li = m 0 (GeV) Li/ 7 Li = m 0 (GeV) He/D = 1 6 Li/ 7 Li = D = m 1/2 (GeV) D = m 1/2 (GeV) Cyburt, Ellis, Fields, KO, Spanos

21 6 Li/ 7 Li = m 3/2 = 0.2m 0, tan β = 10, µ > m 3/2 = 0.2m 0, tan β = 10, µ > 0 3 He/D = 1 3 He/D = 1 7 Li = Li/ 7 Li = Li = 4.3 m 0 (GeV) 0.01 m 0 (GeV) D = 4.0 D = m 1/2 (GeV) m 1/2 (GeV) Cyburt, Ellis, Fields, KO, Spanos

22 A 6 Li Plateau? Observers may not see one, but theorist do predict one! BBN: 6 Li/H ~ Thomas et al. Vangioni et al. Dark Matter: tan = 10 tan = 10 (focus point) tan = 55 tan = 55 (focus point) Jedamzik 6 Li/H abundance BBN m 1/2 [GeV] Ellis et al.

23 Axion Condensation Axion dark matter forms a Bose-Einstein condensate through gravitational self-interactions. Interactions between cold axion fluid cool photon gas: η 10,BBN = ( ) 3/4 2 η 10,WMAP =4.57 ± Li/H ~ 2 x but D/H ~ 4.5 x 10-5 Erken, Sikivie, Tam, Yang

24 Possible sources for the discrepancy Stellar parameters dli dlng =.09.5 Particle Decays dli dt = K Discussed by Ryan Variable Constants

25 How could varying α affect BBN? G 2 FT 5 Γ(T f ) H(T f ) G N NT 2 f Recall in equilibrium, n p e m/t fixed at freezeout Helium abundance, Y 2(n/p) 1+(n/p) If T f is higher, (n/p) is higher, and Y is higher

26 Limits on α from BBN Contributions to Y come from n/p which in turn come from Δm N Contributions to m N : m N aα em Λ QCD + bv Kolb, Perry, & Walker Campbell & Olive Bergstrom, Iguri, & Rubinstein Changes in α, Λ QCD, and/or v all induce changes in m N and hence Y Y Y 2 m N m N α α < 0.05 If α arises in a more complete theory the effect may be greatly enhanced: Y Y O(100) α α α and α < few 10 4

27 Recall, Coupled Variations Campbell and Olive Langacker, Segre, and Strassler Dent and Fairbairn Calmet and Fritzsch Damour, Piazza, and Veneziano α s (M 2 UV ) g2 s(m 2 UV ) 4π = 4π b 3 ln(m 2 UV /Λ2 ) ( mc m b m t Λ = µ µ 3 ) 2/27 exp ( 2π ) 9α s (µ) Λ Λ = R α α ( 3 v v + h c h c + h b h b + h t h t R ~ 30, but very model dependent ) ( Dine et al.

28 Fermion Masses: m f / h f v G F / 1/v 2 Also expect variations in Yukawas, h h = 1 α U 2 α U But in theories with radiative electroweak symmetry breaking v M P exp( 2πc/α t ) Thus small changes in h t will induce large changes in v v v 80 α U α U v v = S

29 Coc, Nunes, Olive, Uzan, Vangioni Dmitriev & Flambaum Approach: Consider possible variation of Yukawa, h, or fine-structure constant, α Include dependence of Λ on α; of v on h, etc. Consider effects on: Q = ΔmN, τn, BD and with h h = 1 α U 2 α U B D B D Q Q τ n τ n = [6.5(1 + S) 18R] α α = ( S 0.6R) α α = [0.2+2S 3.8R] α α,

30 h/h = 0 and Effect of variations of h (S = 160) Mass fraction n 1 H 4 He H He H Li Notice effect on 7 Li Be Time (s) Coc, Nunes, Olive, Uzan, Vangioni

31 S = 240, R = 0, 36, 60, / =2 h/h Mass fraction 3 He/H, D/H He D 3 He For S = 240, R = 36, < h h < Li/H Li x 10-4 h/h Coc, Nunes, Olive, Uzan, Vangioni

32 Finally, h/h = / = 2 h/h, S = 240. Mass fraction He Mass fraction He He/H, D/H 10-5 D 3 He 3 He/H, D/H 10-5 D 3 He 7 Li/H Li 7 Li/H Li S R

33 Summary D, He are ok -- issues to be resolved Li: Problematic - BBN 7 Li high compared to observations Exotic Solutions : - Particle Decays? - Axion Condensate?? - Variable Constants???