Abstract

The Big Bang Nucleosynthesis (BBN) model is a great success of nuclear astrophysics, because of the outstanding agreement between observational and predicted light elements abundances, except for the so-called problem. In this context, experimental efforts to measure the relevant reactions have brought to an increased level of accuracy in measuring primordial abundances and the introduction of indirect methods has allowed to overcome the natural limitations of direct measurements in the energy range of interest for BBN. Here we review the results obtained from the application of the Trojan Horse Method to some of the most influential reactions of the standard network, such as $^2$H(d,p)$^3$H, $^2$H(d,n)$^3$He, $^3$He(d,p)$^4$He, $^7$Li(p,$\alpha$)$^4$He and $^7$Be(n,$\alpha$)$^4$He. The relevant cross sections have been thus used as new inputs of a classical BBN code resulting in important constraints that advice on a possible solution of the lithium problem outside of nuclear physics.

Highlights

  • Big Bang Nucleosynthesis (BBN) occurred when our universe was able to produce nuclei that happened just after the baryogenesis, most probably from the second to the 20th minute after the Bang, while temperature fell from more than 109–108 K

  • Recent and complete reviews for SBBN are given in Cyburt et al (2016) and Pitrou et al (2018). This success relies on the outstanding agreement between what is predicted as the output, namely, the primordial abundances of the elements produced during BBN, and the same abundances resulting from the current observations. This is true for the compliance of nuclear physics and astronomy results and for the model parameters obtained with methods completely outside of nuclear astrophysics, such as the CMB evaluation from the Planck satellite of η · 10−10 = 6.12 ± 0.06 (Planck Collaboration et al, 2018), impressively concordant with the BBN model result of 5.8≤ η · 10−10 ≤6.5, which was given in Cooke et al (2018) and obtained by taking advantage of the most recent and precise measurements of the deuterium primordial abundance

  • These new compilation of direct and Trojan Horse Method (THM) data has led to the numerical calculation of new reaction rates for the reactions in sections above, introducing the R-matrix fits in the reaction rate definition

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Summary

INTRODUCTION

Big Bang Nucleosynthesis (BBN) occurred when our universe was able to produce nuclei that happened just after the baryogenesis, most probably from the second to the 20th minute after the Bang, while temperature fell from more than 109–108 K. This is true for the compliance of nuclear physics and astronomy results and for the model parameters obtained with methods completely outside of nuclear astrophysics, such as the CMB evaluation from the Planck satellite of η · 10−10 = 6.12 ± 0.06 (Planck Collaboration et al, 2018), impressively concordant with the BBN model result of 5.8≤ η · 10−10 ≤6.5, which was given in Cooke et al (2018) and obtained by taking advantage of the most recent and precise measurements of the deuterium primordial abundance With this recent and precise evaluation of η from the Planck mission, it is possible to consider SBBN as a parameter-free model, described with computer programs where outputs are the desired primordial abundances and inputs are the cosmological parameters and the rates of the reactions through which light elements are produced. We discuss the resulting constraints that suggest a possible solution for the lithium problem outside of nuclear physics

NUCLEAR MEASUREMENT PROBLEMS
THM MEASUREMENTS FOR THE BBN SCENARIO
R-Matrix Fit
From TH Data to Reaction Rates
RESULTS
CONCLUSIONS
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