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Big Bang Nucleosynthesis
Karsten JEDAMZIK†
†
LPTA, Montpellier
Karsten Jedamzik, Brussels, December 3rd ‘09 – p.
Outline of Talk
I. Theory of standard BBN
II. Observational determination of primordial light elements
abundances/comparison to standard BBN prediction
III. BBN as a probe of the early Universe and Physics
beyond the standard model
IV. Astrophysical/nuclear physics solutions to the
Lithium problem(s)
V. Beyond the standard model solutions to the lithium
problem(s)
Karsten Jedamzik, Brussels, December 3rd ‘09 – p.
The standard BBN model at Ωb h2 ≈ 0.02273
1
0.01 4
He
1e-04 2
H
3
1e-06 He
ni/np
1e-08 n
1e-10 7
Be
7
1e-12 Li
6
Li
1e-14
1000 100 10
T (keV)
Karsten Jedamzik, Brussels, December 3rd ‘09 – p.
Assumptions underlying Standard Big Bang Nucleosynthesis
general relativity
equilibrium initial conditions
radiation energy density given only by
with baryon−to−photon ratio
photons, electrons/positrons, neutrinos
6.2x10e−10
vanishing lepton number standard no decaying or annihilating
chemical potentials
BBN relic particles
no inhomogeneities in baryons no impurities like
no small antimatter domains cosmic strings, primordial black holes
Karsten Jedamzik, Brussels, December 3rd ‘09 – p.
SBBN: A one parameter model
Ò
Cyburt et al. 08
¿
À À ´½ ¼¼ ¦ ¼ ¼ µ ¢ ½¼ ´ µ
Á º ¿ Ì Ð Ø Ð Ñ ÒØ ÙÒ Ò
× Ó ¸
¿À ¸ Ä Ý ÒÙÑ Ö Û Ø Ö ×Ô
Ø ØÓ À¸ Ò Ø Ñ ××
overconstrained → consistency checks possible
Ö
Ø ÓÒ Ó À × ÙÒ
Ø ÓÒ Ó º Ì Ø
Ò ×× Ó Ø Ò × Ö ÔÖ × ÒØ× ½ ÙÒ
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Ð
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º Ì Ý ÐÐÓÛ Ò Ú × Ø ÏÅ È ¿℄º
Ì Æ ÔÖ
Ø ÓÒ×
Ò
ÓÑÔ Ö Ö
ØÐÝ Û Ø
ÙÖÖ ÒØ Ó × ÖÚ Ø ÓÒ Ð Ø ÖÑ Ò ¹
Karsten Jedamzik, Brussels, December 3rd ‘09 – p.
Ø ÓÒ× Ó Ø Ð Ø Ð Ñ ÒØ ÙÒ Ò
׺ Ì ÆÐ Ð ÓÓ ÙÒ
Ø ÓÒ×
Ò ¬Ò Ý
II. Observational determination of primordial light elements
abundances/ comparison to standard BBN predictions
Karsten Jedamzik, Brussels, December 3rd ‘09 – p.
Helium-4 from low-metallicity extragalactic HII regions
systematic uncertainties
atomic emissivities (changed Yp by
+0.008 !)
temperature variations
ionisation corrections
underlying stellar absorption
Yp = 0.2477 ± 0.0029, 0.2516 ± 0.0011 Peimbert it et. al07, Izotov it et. al07
more realistic error bars: Yp = 0.249 ± 0.009 Olive & Skillman 04
Karsten Jedamzik, Brussels, December 3rd ‘09 – p.
Observational inferred Helium-4 with time
0.26
He mass fraction Yp
0.25
WMAP
0.24
0.23
4
0.22
1990 1995 2000 2005 2010
Year
Karsten Jedamzik, Brussels, December 3rd ‘09 – p.
D/H from Quasar Absorption Systems
Iocco et al. 09
Tytler,Fan,& Burles 96
significant dispersion →
underestimated systematic
º º Ì Ò Ò Ñ ×ÙÖ Ñ ÒØ× Ó µ¹ ܵ ÉË ³× Ù× Ò ÓÙÖ Ò ÐÝ× ×º Ì ÓÖ ÞÓÒØ
+0.29
errors ? Ò Ö ÔÖ × ÒØ× Ø Ú ÐÙ D/H =
Ó Õº ´ 2.98−0.23
µº × 10−5
Ò ¬Ò Ø ÓÐÐÓÛ Ò ÕÙ ÒØ Ø ×
·· ·
·· ´
¾
Karsten Jedamzik, Brussels, December 3rd ‘09 – p.
The 7 Li Spite plateau
-10
4x10
Li/H
3x10-10
2x10-10
-10
1x10
observed Li/H by different groups
Spite & Spite 82, Bonifacio & Molaro 97,
(almost) no variation with metallicity Ryan et al 99, Melendez Ramirez 04, Char-
and stellar temperature bonnel & Primas 05, Asplund et al 06
(almost) no measurable star-to-star
scatter
Interpretation - the Primordial 7 Li
Abundance Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 1
6
Li/H observations
Asplund, Lambert, Nissen, Primas, & Smith
06
6 Liand 7 Li absorption features blend
together
6 Li from asymmetry of lines
asymmetry of lines from convective
Doppler shifts ?
A second Lithium plateau ?
6 non-LTE hydrodynamic simulations of
Li/H ≈ 6 × 10−12 compare to
two groups reach opposite conclu-
standard BBN 6 Li/H ∼ 10−14
sions
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 1
Are the 6 Li detections real ?
Steffen, Cayrel, Bonifacio, Ludwig, & Ö×
Ä Ò Ñ Ø Ð¹ÔÓÓÖ ÐÓ ×Ø Caffau 09 ½¾¿
0.10 Mean : 0.0212
Sigma: 0.0208 0.10 Mean : 0.0059
Sigma: 0.0212
6Li / 7Li isotopic ratio
6Li / 7Li isotopic ratio
0.05 0.05
0.00 0.00
−0.05 −0.05
5800 6000 6200 6400 5800 6000 6200 6400
Teff [K] Teff [K]
Ä » Ä ×ÓØÓÔ
Ö Ø Ó¸ Ò ¦½ ÖÖÓÖ Ö׸ × ÙÒ
Ø ÓÒ Ó «
Ø Ú Ø ÑÔ Ö ØÙÖ ×
ÙÖ ¿º
Ý ×ÔÐÙÒ
Ö Úonly four ∼ 2σ´¾¼¼ µ ÓÖ ´Ð ص Ò Ø Ö ´Ö ص ×Ù ØÖ
Ø ÓÒ Ó ¡Õ´Ä µ ØÓ
ÓÖÖ
Ø
detections Ø Ðº
ÓÖ Ø × Ù ØÓ Ø ÒØÖ Ò×
Ð Ò ×ÝÑÑ ØÖݺ ÐÐ
Ö
Ð × ÒÓØ Ä Ø
Ø ÓÒ× ÓÚ Ø
Ú Ð¸ ÓÔ Ò
Ö
Ð distribution skewed towards positive 6 Li/H
¾ Ð however, × ÒÓØ ÒÓÒ¹ Ø
Ø ÓÒ׺
a positive 6 Li/H detection in HD84937 by four(!) groups
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 1
Helium-3/D
3 He/D < 1.5 for solar system Geiss & Gloeckner 07 is secure and
∼
useful in constraing non-standard BBN Sigl et al. 06
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 1
× Ò Ø ÅÓÒØ ÖÐÓ Ö ×ÙÐØ× ÖÓÑ Æ × ÙÒ
Ø ÓÒ Ó ØÓ Ú Ä Æ´ µ Ò Ø
SBBN Predictions against Observations
ÏÅ È Ú ÐÙ Ó ×ØÖ ÙØ × Ù×× Ò¸ ÄÏÅ È ´ µº Ì × Ö × ÓÛÒ Ò º Ý Ø
Ö ´ ÐÙ µ × Ö ÓÒ׺ Ì ÓÙ Ø Ö Ö Ù× ÙÐ Ñ ×ÙÖ Ñ ÒØ× Ó Ø ¿À ÙÒ Ò
℄¸ Ø × Ö Æ
ÙÐØ ØÓ Ñ Ø
ØÓ Ø ÔÖ ÑÓÖ Ð ÙÒ Ò
℄º Ï Û ÐÐ × ÓÛ Ø Æ
Ð ÓÓ ÓÖ À Ò º ¸ ÙØ Û ÐÐ ÒÓØ ×
Ù×× À ÒÝ ÙÖØ Öº
¿ ¿
Cyburt, Fields, & Olive 08
7x10-10
6x10-10
5x10-10 SBBN + WMAP predicted Li/H
(2−σ -error bars)
-10
4x10
Li/H
-10
3x10
2x10-10
1x10-10
observed Li/H by different groups
7
Li discrepancy 4.2 − 5.3σ
Á º Ì Ø ÓÖ Ø
Ð Ò Ó × ÖÚ Ø ÓÒ Ð Ð Ð ÓÓ ÙÒ
Ø ÓÒ× ÓÖ À ¸ »À¸ ¿ À »À¸ Ò Ä »Àº
Æ Ö ×ÙÐØ× Ú Ò
ÓÒÚÓÐÚ ÛØ Ø ÏÅ È Ø ÖÑ Ò Ø ÓÒ Ó Ò Ö × ÓÛÒ × Ö ´ ÐÙ µ
Ö º Ì Ó × ÖÚ Ø ÓÒ Ð Ð Ð ÓÓ × Ö × ÓÛÒ × Ð Ø ´Ý ÐÐÓÛµ × Ö ÓÒ× × Û ÐÐ ×
Ø ÖÒ Ø Ú ÓØØ
ÙÖÚ ×º Ì Ø Ò ×Ø Ò
Ø ÓÒ× Ö Ø Ð Ò Ø Ø Üغ
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 1
Situation Summary
Element Comparison
4
He ok/inconclusiv
2
H good
3
He inconclusive
7
Li disagreement
6
Li ?
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 1
III. BBN as a probe of the early Universe and Physics
beyond the standard model
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 1
The BBN early Universe Probe
the epoch of BBN is (one) of the furthest back reaching
precision probe of the early Universe
Almost all of the theoretical work in BBN the last three
decades has been done in exploring non-standard
models
changed expansion rate during BBN
lepton chemical potentials
neutrino oscillations, sterile neutrinos, exotic neutrino interactions
baryon inhomogeneous models, matter-antimatter inhomogeneous models
varying fundamental constants
decay and annihilation of relic paticles during BBN
catalysis of BBN
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 1
BBN with decaying and annihilating particles
Jedamzik 04,06
injection of energetic nucleons and mesons 103
102 Bh = 0
charge exchange reactions
101
π− + p → π0 + n 100 -5
-4.5
-1
10 -4
elastic- and inelastic scatterings 2 -3.5
ΩXh 10-2 -3
p + p → p(n) + (p)n + π’s 10-3
-2.5
-2
-1.5
-4
10 -1
spallation reactions 10 -5 0
-0.5 0
p(n) + 4 He → 3 H, 3 He, 2 H + .... 10-6 τ(sec)
-2 0 2
10 10 10 104 106 108 1010 1012
Coulomb stopping of charged nuclei
3 H + e± → 3 H ′ + e±
Kawasaki, Kohri, Moroi 04,06
injection of energetic photons and elec-
trons/positrons
pair production on CMBR
γ + γCMBR → e− + e+
inverse Compton scattering
e± + γCMBR → e± + γ
Bethe-Heitler scattering
γ + p → p + e− + e+
photodisintegration γ + 4 He → 3 H + p
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 1
Example: Supersymmetry, BBN, and Trh
gravitino not LSP → Trh must be low to
avoid too many decays of thermally pro-
duced gravitinos during BBN
gravitino LSP → NLSP decays dangerous
unless τ < 5×103 sec → gravitino LSP some-
∼
what lighter than weak scale → reheat tem-
perature must be low
ÙÖ ½ Ì ÔÐ Ò ´Ñ½ ¾ Ѽ µ ÓÖ Ø Ò ¬ ½¼¸ Ñ Ñ¼ ´Ð
¼ ¾Ñ¼ ´Ö Ø Û Ò ÓÛµ Ò ÓÖ ¼ ¼¸ ¼º Ì Ð Ø ÖÓÛÒ Ö
À × Ö Ü
ÐÙ Ý ÙÒ×Ù
×× ÙÐ
Ö ÒÓ Ò À × × Ö
×
→ supergravity and
Û Ò ÓÛ Ø Ö Ö ÖÓÛÒ Ö ÓÒ Ð Ð × × Ü
ÐÙ
Ì leptogenesis (in most
Ö Ö Ý Ö ÓÒ ÐÓÛ Ø × ÐÒ ×Ð Ð Ì
ÝÓÒ
ÓÑ Ò Ø
ÝÓÒ
¸ Ò × Ð×Ó Ü
ÐÙ º ÁÒ Ø Ö ×Ø Ó Ø Ö Ý
cases) incompatible
×Ø Ù Ñ ×× ÓÙÒ Ñ ½ Î × Ú ÓÐ Ø º ÁÒ Ø Ö ÓÒ ÆÓ
Ö ÒÓØ × Ø ×¬ º Ì ÓØØ ÓÒ Ð Ð Ò Ñ Ö × Ø ÓÙÒ ÖÝ
Ü
ÐÙ Ý Ø Ú Ö ÓÙ× Æ ‘09 – p.
×Ø Ù ´ µ ÆÄËȺ Ì Ö ÓÒ×Karsten Jedamzik, Brussels, December 3rd
ÓÒ×ØÖ1
IV. Astrophysical/nuclear physics solutions to the
lithium problem(s)
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 2
Nuclear reactions/stellar atmospheres ?
stellar temperature ∆T ∼ 900 K underestimated
seems impossible
narrow nuclear resonance in
7 Be +2 H→ 9 B∗ 4
5/2 + → 2 He + p
Cyburt & Pospelov 09, Angulo et al. 05
seems unlikely but not ruled out → need further
measurement
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 2
Depletion of Lithium in PopII stars ?
7 Li
is observed in the atmospheres of PopII stars
it may be destroyed via 7 Li+p →4 He + 4 He in the interieur of
the star
atmospheric material transported into the star and 7 Li-depleted gas returned to the
atmosphere
Spite plateau not primordial ?
Depletion of 7 Li by factor 2 − 4 in halo stars is not understood
and may currently only be explained with fine-tuned stellar
conditions
Dispersion ?
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 2
7
Li depletion by atomic diffusion in PopII stars ?
Korn et al., Richards et al.
atomic diffusion
turbulent mixing
7x10-10
with depletion factor 1.8
-10
6x10
5x10-10 SBBN + WMAP predicted Li/H
(2−σ -error bars)
-10
4x10
Li/H
-10
3x10
2x10-10
1x10-10
observed Li/H by different groups
fine-tuned turbulent diffusion coeffi- → factor 1.8 7 Li depletion
gs ` ρ ´−3
cient DT = 400D4He ρ(T ) at but stellar models ad hoc and tuned
0
log(T0 ) = 6.0 ± 0.1 → ±25%
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 2
6
Li production by early cosmic rays: Energetics ?
6 Lioriginates in galactic cosmic ray nucle- standard cosmic rays may provide
osynthesis (along, with 9 Be, and B) 5 eV/nucleon (up to [Z] ∼ −2.7
via p, α + CNO → LiBeB
and some α + α → Li
only very efficient accretion on central black
hole, or large fraction of baryons in
supermassive ∼ 100M⊙ stars may provide
need 100 eV/nucleon to synthesize
6 Li/H∼ 5 × 10−12
the required cosmic rays
Suzuki & Inoue 00 Rollinde et al. 05,
Prantzos et al. 05 Nath et al. 05
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 2
V. Beyond the standard model solutions to the lithium
problem(s)
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 2
Destruction of 7 Li during BBN due to injection of neutrons
K.J. 04
7
Li destruction: 7 Be +n → 7 Li +p; 7 Li + p →4 He + 4 He
at T ≈ 30 keV
need only 10−5 extra neutrons per baryon
some extra 2 H will be also synthesized
→ possible bydecay/annihilation or relic particles, evaporation
of defects
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 2
Production of 6 Li in cascade nucleosynthesis
6
Li is very easily produced by small "perturbations" of the
standard model Dimopoulos et al. 88, K.J. 00
Electromagnetic:
γ+4 He→ 3 H +p
3
H + 4 He → 6 Li + n
at T < 0.1 keV
∼
Hadronic:
n+4 He→ 3 H +p + n
3
H + 4 He → 6 Li + n
at T < 10 keV
∼
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 2
charged relic - nuclei bound states during/after BBN
Pospelov 06,07, Kohri & Takayama 06, Kaplinghat & Rajaraman 06, Cyburt et al 06, Pradler &
Steffen 06, Hamaguchi et al. 07, Bird, Koopmans, & Pospelov 07, Kawasaki et al. 07,
Takayama 07, Jittoh et al. 07, Jedamzik 07,08
binding energy between nuclei and electrically charged weak
mass scale relics appreciable:
7
Be + τ → (7 Be˜) + γ, 4 He + τ → (7 He˜) + γ, etc.
˜ τ ˜ τ
Bohr radius of bound nuclei between 2 − 4 Fermis
→ formation of bound states towards the end of BBN
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 2
Fraction of nuclei bound to X −
2
Oh = 0.41, Mx = 1 TeV
1
fi
0.1
0.01 7
Be
6
0.001 Li p
7
Li
0.0001
1e-05
4
He
1e-06
time (sec)
1e-07
100 1000 100001000001e+06 1e+07 1e+08
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 2
Production of 6 Li in catalytic nucleosynthesis
negatively charged weak
Pospelov 06,07
mass scale particles X − ½¼
½¼
Ö
¢ ½¼
during BBN → ¢ ½¼¿ ×
½¼ ´ À µ
½¼
formation of bound states ½¼ Ò
Ò ÒÔ
½¼ ½¼ µ
with nuclei ½¼ ½½
´
Ä
7 Be + X − → (7 BeX − ) + γ at ≈ 30 keV ½¼ ½¾
4 He + X − → (4 HeX − ) + γ, at ≈ 10 keV ½¼ ½¿
½¼ ½
½¼ ½
¼½ ¼ ¼¾
−
X acts as catalysator for re- Ì
actions
(4 HeX − ) + D → 6 Li + X − important when Bh < 10−2 as
∼
(4 HeX − ) + 4 He → (8 BeX − ) + γ;
(8 BeX − ) + n → 9 Be + X −
with supersymmetric stau !
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 3
Catalysis and 6 Li, 7 Li, and 7 Be
Catalysis:
main production mechanism for 6 Li if Bh < 10−2
∼
may not solve the 7 Li problem, unless Bh < 10−5 rather
∼
small and ΩX > 10 rather large
∼
not clear if may lead to some 9 Be production
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 3
The lithium friendly parameter space in cascade nucleosynthesis
K.J. 04
D/H
3e-05
Bailly, K.J., Moultaka 08
-1 Yp>0.258
7 10
Li/H
ΩXh2Bh
10-2
1e-10 10-3
-4
D/H>4x10-5
10
10
10-5
6 7
Li/ Li 1
10-6
0.1 2
10 10
3
τ (sec) 10
4
10
5
1e-02
2 3 4 5 6
10 10 10 10 10
τ (sec)
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 3
Signatures at the LHC !
A metastable particle X with life time between
100 − 1000 sec, if not too massive, could be potentially
produced at the LHC (since having at least some hadronic
interactions), and ...., if electromagnetically or strongly
interacting stopped in the detector → smoking gun for
non-standard BBN → possible connection to the dark
matter
Examples:
Gluino in split supersymmetry
supersymmetric stau Next-to-LSP with gravitino LSP
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 3
Example: Gravitino dark matter in the CMSSM
K.J., Choi, Roszkowski, Ruiz de Austri 06
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 3
Solving the 6 Li and 7 Li problems by neutralino annihilation ?
1e-22
1e-23
1e-24
1e-25
1e-26
uu-quark, 6Li/7Li = 0.01-0.09,0.024-0.68; D/H=3.5,4.4,5.3e-5; 7Li/H = 1.5,2,3,4.e-10
1e-27
10 100 1000
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 3
Varying fundamental constants and 7 Li
Dmitriev, Flambaum, & Webb 04, Dent,
Stern, & Wetterich 07, Berengut, Flambaum,
& Dmitriev 09
7 Li depends strongly on Bd and B7 Be
∆Bd /Bd ≈ −0.019 ± 0.005 → reduce 7 Li
(and 4 He)
∆mq /mq ≈ 0.013 ± 0.002 → reduce 7 Li
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 3
Conclusions
the by standard BBN at ηWMAP predicted D (and 4 He) are in good agreement with
those observed
in contrast, there is a factor 3-4 discrepancy between SBBN predicted and
observationally inferred 7 Li
this discrepancy could possibly be removed if 7 Li is destroyed in Pop II stars, though
how this is done exactly is not understood
alternatively BBN could have been non-standard, e.g. including the decay of a relic
particle → potentially testable at the LHC
observations of the existence of a 6 Li plateau (similiar to the 7 Li Spite plateau) are
currently controversial
BBN continous to be a powerful probe of the early Universe and physics beyond the
standard model
Karsten Jedamzik, Brussels, December 3rd ‘09 – p. 3
