How accurately can the deuterium abundance be determined ?

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dc.creatorLevshakov, S. A.
dc.creatorKegel, W. H.
dc.creatorTakahara, F.
dc.date1997-08-07
dc.date.accessioned2026-07-07T02:23:58Z
dc.date.available2026-07-07T02:23:58Z
dc.descriptionBy using a Reverse Monte Carlo technique aimed at the inverse problem in the analysis of the H+D Ly-a absorption from QSO spectra we have estimated the physical parameters of the gas and the large-scale line of sight velocity structure towards Q1009+2956 at z = 2.504 (observations by Burles and Tytler, astro-ph/9603070). We show that for a precise evaluation of the column densities, the detailed velocity field structure is to be determined simultaneously. Our study of the z = 2.504 system yields D/H = (3.75 +/- 0.85)*10^{-5} (2sigma) which gives good agreement between the standard BBN predictions and observational constraints on extra-galactic 4He mass fraction and 7Li abundances in the atmospheres of population II (halo) starts. We conclude that the discordance of D/H with the light element abundances discussed in the literature is a consequence of the assumption of microturbulence (i.e. completely uncorrelated bulk motions) in the analysis of line profiles. The generalized model accounting for a finite correlation length leads to the common eta-interval of (3.9-5.3)*10^{-10}, where eta is the baryon to photon ratio.
dc.description4 pages, 2 Postscript figures, uses conf_iap.sty A contribution to the Proceed. 13th IAP Colloquium "Structure and Evolution of the IGM from QSO Absorption Line Systems" (Paris, July 1-5, 1997)
dc.identifierhttps://arxiv.org/abs/astro-ph/9708064
dc.identifierhttp://arxiv.org/abs/astro-ph/9708064
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/11455
dc.subjectAstrophysics
dc.titleHow accurately can the deuterium abundance be determined ?
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