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 (D/H) max ~ 0.7·10 -2 kT BBN ~ 70 keV n B (BBN) ~ cm -3 n  (BBN) ~ cm -3

Physical Parameters Our Epoch BBN Epoch t ~ 14 Gyrt ~ 3-5 m T 0 = K (1+z 0 ) = 1 T B = 0.8  10 9 K (1+z B ) = 3.0  10 8 n  = 411 cm -3   = 0.26 eV cm -3 n  = cm -3   = 2  eV cm -3 n B = 4.11   10 cm -3  B = 39  10 eV cm -3 n B =  10 cm -3  B =  10 eV cm -3  10  (n B /n  ) = 6.0  0.5 (CMBR)

BBN Yield: Light Nuclei Abundances Standard Model n B ( BBN ) is the only free parameter [D] is the most sensitive to n B (BBN) Under Adiabatic Expansion Fraction of Baryon Matter The Standard Matter Fraction is ~ 5% !!! M H /M B ~0.76 M He4 /M B ~0.24 M Z /M B <10 -4 Contemporary density

CMBR: T 0 =2.726 K,   (0)=0.26 eV/cm 3, n  (0)=411 cm -3 Redshifted Thermal Radiation of the Primordial Plasma at the Recombination Epoch: t R ~ yr, T R ~ 3000 K, n B (R) ~ 300 cm -3, n  (R) ~5·10 11 cm -3 Anisotropy of CMBR CMBR fluctuations  T 0 /T 0 ~10 -5 display a beginning stage of LSS formation. Correlation of the fluctuations Comparison of the theory with observations by WMAP gives: Power spectrum of CMBR fluctuations

Angular size dependencies on the Space Curvature

DI/HI Atomic Lines in QSO Absorption Spectra Ly   ÅH I ÅD I  (H I) /  (D I) = [D I] / [H I] (2.0±0.5)   Webb et al (2.6±0.4)   Kirkman et al Primordial Nucleosynthesis  n B /n      h 2  Const(t)  B  0.044±0.004 (Burles et al. 2001) Difficulties of DI/ HI line identification

European South Observatory : Very Large Telescope

H 2 absorption lines imprinted in QSO spectrum (z abs = ) Varshalovich, Ivanchik, Petitjean et al., Astron Letters 27, 683, 2001

HD absorption lines imprinted in QSO spectrum (z abs = )

Interstellar Molecular Clouds 12 Gyr ago: [H 2 ] ~ 4.8·10 19 cm -2 [HD] ~ 3.4·10 15 cm -2 Our Epoch: [H 2 ] ~ 3.4·10 20 cm -2 [HD] ~ 2.1·10 14 cm -2

Molecular cloud at z= n Molecular column densities n HD/H 2 molecular abundance ratio n The limit of HD/H 2 chemistry: D/H isotope ratio

D/H relative abundances: QSO observational data

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

Observed and predicted BBN abundances 4 He 2 D 3 He 7 Li CMBR After Big Bang BBN 3-5 min CMBR 3.8  10 5 yr QSO Abs. 8.5  10 8 yr Our Galaxy 1.4  yr D is destroyed in stars: D/H decreases during galaxy evolution with cosmological time

Conclusions I n n HD-molecules at high redshift are detected for the first time. n n Primeval H 2 -HD molecular cloud was discovered that had existed 12 Gyr ago. n n The ratio of [HD]/[H 2 ] in the primeval cloud was significantly larger than that is observed in the interstellar clouds of our Galaxy.

n We obtain D/H isotope ratio by independent method from HD/H 2 abundances and include it into the BBN code. The result is n The fraction of baryon matter at our epoch is which coincides (within the errors) with  B from CMBR WMAP Conclusions II

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

Н 2 rotational level populations N J=5 = (2.3±0.3)   cm -2 N J=4 = (5.0±0.6)   cm -2 N J=3 = (2.3±0.5)   cm -2 N J=2 = (6.0±3.0)   cm -2 N J=1 = (1.9±0.1)   cm -2 N J=0 = (2.8±0.1)   cm -2 N(H 2 ) =  N J = = (4.8±0.2)   cm -2

Radiative transfer of H 2 lines

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

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