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BBN Epoch: Evolution of Nuclear Composition

Первичный нуклеосинтез , образование D и содержание HD/H 2 в межзвездных облаках, существовавших 12 млрд. лет назад Д . А. Варшалович , А.В. Иванчик , С.А. Балашев Физико-технический институт им. А.Ф. Иоффе РАН 2009. BBN Epoch: Evolution of Nuclear Composition. t ~ 3-5 min

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BBN Epoch: Evolution of Nuclear Composition

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  1. Первичный нуклеосинтез, образование D и содержание HD/H2 в межзвездных облаках, существовавших 12 млрд. лет назадД.А.Варшалович, А.В. Иванчик, С.А. БалашевФизико-технический институт им. А.Ф. Иоффе РАН2009

  2. BBN Epoch: Evolution of Nuclear Composition t ~ 3-5 min (D/H)max ~ 0.7·10-2 kTBBN ~ 70 keV nB(BBN) ~ 1018-1019cm-3 ng(BBN) ~ 1028cm-3

  3. BBN Yield: Light Nuclei Abundances MH/MB~0.76 MHe4/MB~0.24 MZ/MB<10-4 • Standard Model • nB(BBN)is the only free parameter • [D] is the most sensitive to nB(BBN) • Under Adiabatic Expansion • Fraction of Baryon Matter • Contemporary density The Standard Matter Fraction is ~ 5% !!!

  4. CMBR: T0=2.726 K, eg(0)=0.26 eV/cm3, ng(0)=411 cm-3 Redshifted Thermal Radiation of the Primordial Plasma at the Recombination Epoch: tR ~ 400000 yr, TR ~ 3000 K, nB(R) ~ 300 cm-3, ng(R) ~5·1011 cm-3 Power spectrum of CMBR fluctuations Anisotropy of CMBR CMBR fluctuations dT0/T0~10-5 display a beginning stage of LSS formation. Correlation of the fluctuations Comparison of the theory with observations by WMAP gives:

  5. Angular size dependencies on the Space Curvature

  6. DI/HI Atomic Lines in QSO Absorption Spectra PrimordialNucleosynthesis Difficulties of DI/ HI line identification • = nB/ng = 2.74´10-8 WBh2 = Const(t) • WB= 0.044±0.004 (Burles et al. 2001)

  7. European South Observatory : Very Large Telescope

  8. H2absorption lines imprinted in QSO 1232+082 spectrum (zabs = 2.33771) Varshalovich, Ivanchik, Petitjean et al., Astron Letters 27, 683, 2001

  9. HD absorption lines imprinted in QSO 1232+082 spectrum (zabs = 2.33771)

  10. Interstellar Molecular Clouds 12 Gyr ago: [H2] ~ 4.8·1019 cm-2 [HD] ~ 3.4·1015cm-2 Our Epoch: [H2] ~ 3.4·1020 cm-2 [HD] ~ 2.1·1014cm-2

  11. Molecular cloud at z=2.33771 • Molecular column densities • HD/H2 molecular abundance ratio • The limit of HD/H2 chemistry: D/H isotope ratio

  12. D/H relative abundances: QSO observational data

  13. BBN Theory • Baryon/Photon number density ratio corresponding to the D/H isotope ratio • Under Adiabatic Expansion • So, the number density of baryons (average) at our epoch The average fraction of baryon matter at our epoch is

  14. Observed and predicted BBN abundances 4He 2D 3He 7Li CMBR

  15. Conclusions I • HD-molecules at high redshift are detected for the first time. • Primeval H2-HD molecular cloud was discovered that had existed 12 Gyr ago. • The ratio of [HD]/[H2] in the primeval cloud was significantly larger than that is observed in the interstellar clouds of our Galaxy.

  16. Conclusions II • We obtain D/H isotope ratio by independent method • from HD/H2 abundances and include it into the BBN code. • The result is • The fraction of baryon matter at our epoch is which coincides (within the errors) with B from CMBR WMAP

  17. Conclusions III • Nevertheless, our most probable D/H value is a bit larger than the one commonly accepted today. • This value is in better agreement with other observational data, including 4He, 3He, 7Li.

  18. Н2rotational level populations

  19. Radiative transfer of H2 lines

  20. Changing populations of levels with optical depth Balashev, Varshalovich, Ivanchik, Astron Letters 35, 150, 2009

  21. Nonstandard curves of growth Balashev, Varshalovich, Ivanchik, Astron Letters 35, 150, 2009

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