2 Lithium Problems. Lithium Update

Transcription

1 Lithium Update

2 2 Lithium Problems Lithium Update

3 Lithium Update 2 Lithium Problems - BBN overproduction of 7 Li

4 Lithium Update 2 Lithium Problems - BBN overproduction of 7 Li - GCRN underproduction of 6 Li

5 Lithium Update 2 Lithium Problems - BBN overproduction of 7 Li - GCRN underproduction of 6 Li

6 Lithium Update 2 Lithium Problems - BBN overproduction of 7 Li - GCRN underproduction of 6 Li Lithium Solutions?

7 Lithium Update 2 Lithium Problems - BBN overproduction of 7 Li - GCRN underproduction of 6 Li Lithium Solutions? - Post BBN Particle Decay

8 Lithium Update 2 Lithium Problems - BBN overproduction of 7 Li - GCRN underproduction of 6 Li Lithium Solutions? - Post BBN Particle Decay. claims to solve both problems

9 Lithium Update 2 Lithium Problems - BBN overproduction of 7 Li - GCRN underproduction of 6 Li Lithium Solutions? - Post BBN Particle Decay. claims to solve both problems - Cosmological Cosmic Rays

10 Lithium Update 2 Lithium Problems - BBN overproduction of 7 Li - GCRN underproduction of 6 Li Lithium Solutions? - Post BBN Particle Decay. claims to solve both problems - Cosmological Cosmic Rays. massive Pop III CR production of 6 Li

11 Big Bang Nucleosynthesis Production of the Light Elements: D, 3 He, 4 He, 7 Li 4 He observed in extragalctic HII regions: abundance by mass = 25% 7 Li observed in the atmospheres of dwarf halo stars: abundance by number = D observed in quasar absorption systems (and locally): abundance by number = 3 x He in solar wind, in meteorites, and in the ISM: abundance by number = 10-5

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13 WMAP best fit (WMAPext + 2dFGRS + Lyman α +running sp. index ) Ω B h 2 = ± η 10 = 6.14 ± 0.25

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15 D/H abundances in Quasar apsorption systems Q Q Q PKS

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18 4 He Measured in low metallicity extragalactic HII regions (~100) together with O/H and N/H Y P = Y(O/H 0) He is Primordial! Y O/H

19 Y p Y p = ± Y IT 98 OS !! 1 O/H x 10 4

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22 Li/H Measured in low metallicity dwarf halo stars (over 100 observed) [Li] 2.0 [Li] T (K) [Fe/H]

23 Li Woes Observations based on - old : Li/H = 1.2 x Spite & Spite + - Balmer: Li/H = 1.7 x Molaro, Primas & Bonifacio - IRFM: Li/H = 1.6 x Bonifacio & Molaro - IRFM: Li/H = 1.2 x Ryan, Beers, KAO, Fields, Norris - Hα (globular cluster): Li/H = 2.2 x Bonifacio et al. - Hα (globular cluster): Li/H = 2.3 x Bonifacio - λ6104: Li/H ~ 3.2 x Ford et al. Li depends on T, ln g, [Fe/H], depletion, post BBN-processing,... Strong systematics

24 Problem 1: BBN 7 Li too high

25 Possible sources for the discrepancy Stellar Depletion - lack of dispersion in the data, 6 Li abundance - standard models (<.05 dex), models ( dex) Nuclear Rates - Restricted by solar neutrino flux Vauclaire & Charbonnel Pinsonneault et al. Coc et al. Cyburt, Fields, KAO Stellar parameters dli dlng =.09.5 dli dt = K

26 Reappraising the Spite Lithium Plateau: Extremely Thin and Marginally Consistent with WMAP Jorge Meléndez 1 and Iván Ramírez 2 New evaluation of surface temperatures in 41 halo stars with systematically higher temperatures ( K) [Li] = 2.37 ± 0.1 Li/H = 2.34 ± 0.54 x 10-10

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32 D, He and Li Cyburt, Ellis, Fields, KAO

33 All Cyburt, Ellis, Fields, KAO

34 -5 6 Li/ 7 Li 6 Li Log [! x (GeV)] -10 D 7 Li 4 He D Log [" x (sec)] Jedamzik Feng et al. Ellis, KAO, Vangioni

35 m 0 200! NSP < 10 4 s Regions in the plane with 200 Li/H < 3 x m r < Blue: D/H > 1.3 x 10-5 Red: D/H > 2.2 x m 1/2 (GeV) m 1/2 (GeV) r < mm 3/2 3/2 = = GeV m 0, tan " = 10, µ > m 3/2 = m 0, tan " = 10, µ > m 0 (GeV) ! NSP < 10 4 s r < 1 m 0 (GeV) r < 1! NSP < 10 4 s m 1/2 (GeV) 100 r < 1! NSP < 10 4 s m 1/2 (GeV) Figure 3: The (m 1/2, m 0 ) planes for µ > 0, tan β = 10 and (a) m 3/2 = 10 GeV, (b) m 3/2 = 100 GeV, (c) m 3/2 = 0.2m 0 and (d) m 3/2 = m 0. We restrict our attention to the Ellis, KAO, Vangioni

36 Regions in the plane with Li/H < 3 x Blue: D/H > 1.3 x 10-5 Red: D/H > 2.2 x ^ A = 3 - ˆ3; µ > ^ A = 2; µ > m 0 (GeV) m 0 (GeV) r < r < m 1/2 (GeV) m 1/2 (GeV) Ellis, KAO, Vangioni

37 Blue: D/H > 1.3 x 10-5 Red: D/H > 2.2 x Log [! x (GeV)] Count Log [" x (sec)] Ellis, KAO, Vangioni

38 Blue: D/H > 1.3 x 10-5 Red: D/H > 2.2 x Log [! x (GeV)] Log [" x (sec)] 7Count Count He/D Ellis, KAO, Vangioni

39 Blue: D/H > 1.3 x 10-5 Red: D/H > 2.2 x Log [! x (GeV)] Log [" x (sec)] 7Count Count Require 3 He/D < He/D Ellis, KAO, Vangioni

40 -5 6 Li/ 7 Li 6 Li Log [! x (GeV)] -10 D 7 Li 4 He D Log [" x (sec)] Ellis, KAO, Vangioni

41 -5 6 Li/ 7 Li 6 Li Log [! x (GeV)] -10 D 7 Li 4 He D 3 He/D Log [" x (sec)] Ellis, KAO, Vangioni

42 6 Li In the happy but not too distant past: 6 Li (@ [Fe/H] 2.3): SFOSW HD 84937: 6 Li/Li = ± BD 26 o 3578: 6 Li/Li = 0.05 ± 0.03 SLN Hobbs & Thorburn cf. BBN abundance of about 6 Li/H = or 6 Li/Li < 10-4 Cayrel etal

43 These data nicely accounted for by Galactic Cosmic Ray Nucleosynthesis Fields and Olive Vangioni et al.

44 Problem 2: There appears to be a 6 Li plateau log ( 6 Li/H), log (Li/H) Li/H 6 Li/H [Fe/H] Data from Asplund et al and Inoue

45 Solution 1: Particle Decays D/H 3e-05 7 Li/H 1e Li/ Li 0.1 1e ! (sec) Jedamzik Kawasaki, Kohri, Moroi

46 Solution 1: Particle Decays Kawasaki, Kohri, Moroi

47 Jedamzik et al.

48 Li D Li D Preliminary 3 He A Am1/2 m1/2 Solution 1 plagued by the overproduction of D/H. Cyburt, Ellis, Fields, Olive, Spanos

49 Solution 2: Cosmological Cosmic Rays (to Problem 2 only) Montemerle Cosmic Chemical Evolution Early Reionization and Massive Stars Cosmic Ray Production and Propagation in an expanding Universe Montemerle N l,h (E,z) t = σ αα l (E,E )n He (z)φ α,h (E,z)dE Φ α,h (E,z) = φ α(e) n 0 H β φ α (E s ) β φ α (E) dz dt zs exp(!ξ) b(e,z s ) 1 z / E E s (4) φ α (E) = F 12.5K αp (E + E 0 ){E(E + 2E 0 )}!(γ+1)/2 Rollinde. Vangioni, Olive

50 Daigne, Olive, Silk, Stoehr, Vangioni

51 SNR log(cr p) [ergs / Mpc3 / yr] [number / Mpc3 / yr] Model 1 (Pop III) Model 1e Model 1 (total) Model 1 (Pop II) E SN (z) = (1+z) 3 msup Rollinde. Vangioni, Olive redshift, z max(8m,m min(t) ) dmφ(m)ψ(t!τ(m))e CR (m). (9) E CR (m) = ɛe cc(m) 100 ɛ =

52 Li/H log ( 6 Li/H), log (Li/H) 6 Li/H [Fe/H] Rollinde. Vangioni, Olive

53 Summary D, He are ok -- issues to be resolved Li: 2 Problems - BBN 7 Li high compared to observations - BBN 6 Li low compared to observations 6 Li plateau? Important to consider: - Depletion - Li Systematics - T scale - Particle Decays? - PreGalactic production of 6 Li