25-29 January 2016
Bormio, Italy
Europe/Berlin timezone

Study of the 2H(p,γ)3He reaction in the BBN energy range at LUNA

25 Jan 2016, 17:39
Bormio, Italy

Bormio, Italy

Poster Nuclear Structure and Astrophysics Monday Afternoon


Dr Viviana Mossa (INFN sez. di Bari - Università degli studi di Bari)


The Big Bang Nucleosynthesis (BBN) describes the production of light nuclides in the first minutes of cosmic time. It started with deuterium accumulation when the Universe was cold enough to allow 2H nuclei to be survived to photo-disintegration. A primordial deuterium abundance evaluation D/H=(2.65±0.07)×10^(-5) [1] is obtained by merging BBN calculations and CMB analysis obtained by the Planck collaboration. This value is in tension with the astronomical observations on metal-poor damped Lyman alpha systems, according to which D/H=(2.53±0.04)×10^(-5) [2]. The main source of uncertainty on standard BBN prediction of deuterium abundance is actually due to the radiative capture process 2H(p,γ)3He converting deuterium into helium, because of the poor knowledge of its S-factor at BBN energies. A measurement of this reaction cross section is thus desirable with a 3% accuracy in the energy range 10keV

Primary author

Dr Viviana Mossa (INFN sez. di Bari - Università degli studi di Bari)

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