Constraintson B from StandardBigBangNucleosynthesis (SBBN) and - - PowerPoint PPT Presentation

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constraints on b from standard big bang nucleosynthesis
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Constraintson B from StandardBigBangNucleosynthesis (SBBN) and - - PowerPoint PPT Presentation

Mar 22, 2023 240 likes •530 views

Constraintson B from StandardBigBangNucleosynthesis (SBBN) and CMBobservations AlainCoc (CSNSM,Orsay), ElisabethVangioni-Flam(IAP,Paris), PierreDescouvemontand AbderrahimAdahchour

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SLIDE 1

ConstraintsonΩBfrom StandardBigBangNucleosynthesis (SBBN) and CMBobservations

AlainCoc (CSNSM,Orsay), ElisabethVangioni-Flam(IAP,Paris), PierreDescouvemontand AbderrahimAdahchour (ULB,Bruxelles), andCarmenAngulo(UcL,Louvain-la-Neuve)

  • DeterminationsofΩB(SBBN,CMB)
  • Observationaldata(7Li,Dand4He)
  • Nucleardata(recentcompilations)
  • ComparisonsofΩBranges anddiscussion
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SLIDE 2

DensitycomponentsoftheUniverse Anaturalreference:thecriticaldensity :

G H

C

π ρ 8 3

2

=

=1.88h2× 10-29 g/cm3or 2.9h2× 1011 M

  • /Mpc3

Numberofbaryonsperphoton: η ≡ nb/nγ et Ωbh2=3.65×107η

(h=H0/100km/s/Mpc h=0.71)

Ω≡ρ/ρC

~0.002 ΩL Visiblematter 0.044±0.004 Ωb Baryons 1.02±0.02 ΩT Total 0.73±0.04 ΩΛ Vacuum 0.27±0.04 Ωm Matter

SomeΩ values

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SLIDE 3

q StandardBigBangNucleosynthesis Calculatedandobserved4He,D,3He,7Li primordialabundances

✁

η (or ΩBh2) Needgood:

Observationaldata Nucleardata

Ωbdetermination

q AnisotropiesintheCosmicMicrowaveBackgroundradiation

BOOMERanG,CBI,DASI,MAXIMA,ARCHEOPS,WMAP,…..

q HIandHeII Lyman-α forestabsorption(onthelineof sightofquasars)

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SLIDE 4

AnisotropiesoftheCosmicMicrowaveBackground(CMB)

FollowingCOBE,newgenerations

  • finstruments(BOOMERanG,

CBI,DASI,MAXIMA, ARCHEOPS),nowWMAP and soonPlankSurveyor arededicated tothestudyofCMBanisotropies. Att≈0.3Ma,andT≈3000K: recombination,theUniversebecomes transparent(presently2.725K)

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SLIDE 5

Spatialfluctuationspectrum ofCMB→ (Inertia ofbaryons) Geometry (ΩT≈1),1st peak ΩB (2nd/1st peaks)

ΩBh2=0.0224±0.0009 η=6.134±0.246

[WMAP: Spergel etal.(2003)]

AnisotropiesoftheCosmicMicrowaveBackground(CMB)

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SLIDE 6

Best isotopetoconstrainη ?

4He :littlesensitivetoη 3He :stellarproduction/

destructionnotwellunderstood.

7Li :maindrawback:anon

monotonicevolutionwithη; twoη valuesforagivenLi/H D :seemsthebestcandidate:a strongmonotonicevolutionwith η andnostellarproduction.

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SLIDE 7

Deuteriumprimordialabundance

Fragileisotope:onlydestroyedafterBBN

✁

usehighestobservedvalue

  • 1. Localinterstellarmedium(present):

D/H=1.510-5

  • 2. Protosolar cloud(4.6Gyr ago):

D/H=2.110-5

  • 3. Remotecosmologicalclouds onthe

lineofsightofquasars

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SLIDE 8

D/Hobservationsina cosmologicalcloud Cloudatredshift ofz =3.6

  • nthelineofsightof

quasarQSO1937-1009 D

Lyman-α forest

Observations:

  • D/Hratioathighredshift

fromthedepth/widthof absorptionlines

  • Baryonicdensity(Ωb)from

thecensusofthe«Lyman-α Forest » lines

[Burles &Tytler 1998]

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SLIDE 9

2002 2003

Burles &Tytler 1998;Tytletetal.1996;O’Meara etal.2001; D’Odorico etal.2001;Pettini &Bowen2001;Kirkmanetal.2003

D/Hobservationsincosmologicalclouds

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SLIDE 10

Observationoflithiumabundancesinlowmetallicity stars

  • Spiteplateau:Li/Hversusmetallicity (time)

[Spite&Spite,1982]

  • Lowdispersion
  • 6Liobservations

(6Li/7Li≈10-2)

[Cayrel etal.,1999]

✂

lowLidestruction

✂

Reliableprimordial abundance

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SLIDE 11

Deducedprimordialabundance:Li/H=(0.91–1.91)×10-10 after correctionforsystematiceffects[Ryanetal.,2000]

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SLIDE 12

4Heobservationsin

bluecompactgalaxies

Fromasampleof82HIIregions in76bluecompactgalaxies: Yp=0.2421±0.0021 [Izotov &Thuan 2003] Previouslyusedvalues :

  • Yp=0.2452±0.0015

[Izotov etal.(1999)]

  • Yp=0.2391±0.0020

[Peimbert etal.(2002)]

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SLIDE 13

Primordialnucleosynthesis withη10=1et10

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SLIDE 14

Newexperiments:

  • 3He(n,p)3H:3H(p,n)3Heby

[Brune etal.1999]

Compilations….

  • NACRE[Angulo,Arnould,

Rayetetal.(1999)]

  • SKM93[Smith,Kawano &

Malaney (1993)]

The12reactionsofstandard BBN Newcompilation:

[Descouvemont,Adahchour, Angulo,Coc &Vangioni- Flam (2003),submitted]

Originofreactionrates Theoretical:

  • n↔p:withτn=886.7±1.9s

[PDG2000],verysmall uncertainty[Brown& Sawyer(2001)]

  • 1H(n,γ)2H:Twonucleons

effectivefieldtheory[Chen &Savage(1999)]

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SLIDE 15

Dataevaluationforthe7Li(p,α)4Hereaction

Polynomialfitofselecteddata [Angulo etal.NP1999] Spline fitofalldata [Nollett &Burles,PRD2000] [Smithetal. ApJ 1993]

(Seealso Cyburt,Fields & Olive,2001)

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SLIDE 16

Newanalysisof BBNrates

[DAACV]Descouvemont, Adahchour, Angulo, Coc & Vangioni-Flam (2003), submitted

« R-Matrix »formalism: S-factorsfitsofdata constrainedbytheory

NACRE

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SLIDE 17

∆Y/Y≡ Y(highrate)/Y(lowrate)-1 (maximumfor 1≤η10≤10)

  • ≡|∆Y/Y|< 0.01

Influenceofnuclearuncertainties

  • 0.13
  • ±1σ

SKM (1993)

7Be(n,p)7Li

  • 0.25
  • H/L

NACRE(1999)

7Li(p,α)4He

0.39

  • H/L

NACRE(1999)

3He(α,γ)7Be

  • 0.12
  • 0.12
  • ±1σ

SKM (1993)

3He(d,p)4He

  • 0.03
  • 0.06
  • ±1σ

B (1999)

3He(n,p)3H

0.24

  • H/L

NACRE(1999)

3H(α,γ)7Li

  • 0.07
  • H/L

NACRE(1999)

3H(d,n)4He

0.01

  • 0.04
  • 0.03
  • H/L

NACRE(1999)

2H(d,p)3H

0.12 0.06

  • 0.09
  • H/L

NACRE(1999)

2H(d,n)3He

0.26 0.19

  • 0.19
  • H/L

NACRE(1999)

2H(p,γ)3He

0.08

  • Theory

CS(1999)

1H(n,γ)2H 7Li 3He

D

4He

limits Ref. Reaction/∆Y/Y

log(XH/XL)|MAX ≡log(X(rate+1σ)/X(rate-1σ)) (maximumfor 1≤η10≤10)

  • ≡ |log(XH/XL)|MAX< 0.001
  • 0.003
  • ±1σ

DAACV(2003)

7Be(n,p)7Li

  • 0.039
  • ±1σ

DAACV(2003)

7Li(p,α)4He

0.049

  • ±1σ

DAACV(2003)

3He(α,γ)7Be

  • 0.004
  • 0.006
  • ±1σ

DAACV(2003)

3He(d,p)4He

  • 0.017
  • 0.018
  • ±1σ

DAACV(2003)

3He(n,p)3H

0.038

  • ±1σ

DAACV(2003)

3H(α,γ)7Li

  • 0.004
  • 0.003
  • ±1σ

DAACV(2003)

3H(d,n)4He

0.003

  • 0.008
  • 0.008
  • ±1σ

DAACV(2003)

2H(d,p)3H

0.011 0.007

  • 0.009
  • ±1σ

DAACV(2003)

2H(d,n)3He

0.034 0.022

  • 0.030
  • ±1σ

DAACV(2003)

2H(p,γ)3He

log(XH/XL)|MAX (XH-XL)MAX

7Li 3He

D

4He

limits Ref. Reaction/∆Y/Y

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SLIDE 18

Comparisonbetween

  • bservedandcalculated

abundances Limits(1-σ)obtainedby Monte-CarlofromDAACV reactionrateuncertainties.

  • D:D/H=(2.78+0.44
  • 0.38)×10-5 (1σ)

[Kirkman etal.(2003)]

  • 7Li:Li/H=(1.23+0.68
  • 0.32)×10-10 (2σ)

[Ryan etal.(2000)]

  • ΩBh2=0.0224±0.0009,[WMAP:

Spergel etal.(2003)] Primordialabundances

  • 4He:Yp=0.2452±0.0015 [Izotovetal.

(1999)], Yp=0.2391±0.0020 [Peimbert etal.(2002)] Primordialabundances

  • 4He:Yp=0.2421±0.0021

[Izotovetal.(2003)]

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SLIDE 19

η10 =6.134±0.246 (WMAP) SBBN+(D,Li,4He),95%c.l.: 5.0<η10<7.3 (D only) 1.6<η10<4.3 (Lionly) 2.45<η10<5.20 (4Heonly) 2.45<η10<4.20 (Li&4He)

Baryonicdensity:CMBvs SBBN?

D+Li (68%c.l.)

P r

  • v

i s i

  • n

a l

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SLIDE 20

PrimordialabundancesfromCMBvalueofΩbh2andSBBN

  • D/H=(2.66±0.17)×10-5 (1σ)

FullycompatiblewithD/H measuredvaluesincosmological clouds.

  • Li/H=(4.18±0.46)×10-10 (1σ)

Afactorof≈ 3.4higherthanthe valuededucedfromobservations UsingΩBh2=0.0224±0.0009, [WMAP: Spergel etal.(2003)] and DAACV ratesinSBBNcalculations give: Seealso Cyburt,Fields & Olive, astro-ph/0302431(≈NACRE)

D/H=(2.74+0.26

  • 0.16)×10-5 (1σ)

Li/H=(3.76+1.03

  • 0.38)×10-10 (1σ)
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SLIDE 21

OriginofCMB/SBBNdiscrepancies?

  • Stellar?

Observationalbias:1D/3D,LTE/NLTEmodel atmospheres Listellardestruction(6Liobservations,however)

  • Cosmology?

ExtensionofGeneralRelativity,Quintessence, Branes,Leptonasymmetry,InhomogeneousBBN, Variationoffundamentalcouplings,…. Blazars contaminationofCMB[astro-ph/0306206]

  • Pregalactic evolution?(notaffectingD!)

Spallation bycosmologicalcosmicrays Firstgenerationstars

  • Nuclear?

Variationofα

[Nollett &Lopez 2002]

Variationofα

[Nollett &Lopez 2002]

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SLIDE 22

Experimentaldataon10B(p,α)7Bereaction

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SLIDE 23

Evolutionofthe10B(p,α)7Berate

Theratiobetweenthe NACRE (Angulo etal., 1999)rateandtheCF88 (Caughlan &Fowler, 1988)one. Afactorof≈10inthe SBBNproductionof10B Reactionratescanchangebyhugefactorsfromoldestimatesto newones(newdata).Anotherexample18F(p,α)innovae.

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SLIDE 24

Othernuclearreactionrates

Significantchanges(upto×3) for:3H(p,γ)4He,7Be(n,α)4He and7Li(d,n)24He butnotallowed and/oraffectslowdensityregion Aninterestingcase: the7Be(d,p)2α reaction

←×30 ←×100 ←×300 ←×1000

Othernuclearreactionrates

  • About100otherreactions

involvedinSBBNfromHtoB

  • Amongthem≈40remainwhose

uncertaintyonrateisnotavailable

  • Systematiccheckbyvaryingthe

ratesbyfactorsof10,100,1000.

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SLIDE 25

Experimentaldataon7Be(d,p)2α reaction

Reactionrate[CF88] from anestimate[Parker,1972] basedonpartialexperimental data[Kavanagh,1960] NodataatBBNenergies!

7Be(d,p)8Be*→2α

Experiment(2004)

Experimentin2004 at LouvainlaNeuve 1. Reversekinematics:7Bebeam(Louvain laNeuve)andCD2 target. (CRC(LouvainLN),CSNSM,Edinburgh,ULB) 2. Directmeasurementradioactive7Be target andd beam(CENBG2005?)

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SLIDE 26

8Be+p 5Li+α

Kavanagh1960

? ?

The7Be(d,p)2α and7Be(d,α)5Lireactions

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SLIDE 27

Conclusions

  • FirstSBBNcalculationswith« main »nuclearreactionrates
  • ConstrainedbyR-matrixtheory
  • Statisticallyevaluateduncertainties
  • Confirms good agreementforΩB valuesdeducedfrom:

1. CMB, 2. SBBN(D), 3. Lyman-α

  • Howeverdisagreementbetween :

v SBBN(7Li+4He)andCMB

  • Stellar,cosmology,pre-galactic,origin?
  • Needtoexcludenuclearorigin

v Systematicerrors[e.g.3He(α,γ)7Be)] butnotafactorof3!!! v Investigate« new »SBBNreactions[7Be+d ]

  • Maybesomeinterestingnew(astro)physics