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The direct measurement of the $^{6}Li$$\it{(p}$,$\alpha$)$^{3}He$ reaction at astrophysical energies using the scaled-down version of the ELISSA array has been performed at the IFIN-HH 3MV Tandetron. The $^{6}Li$$\it{(p}$,$\alpha$)$^{3}He$ reaction plays a key role in stellar nucleosynthesis, being tightly bound to the well-known "Cosmological Lithium Problem" for it takes place in the context of the lithium depletion mechanisms in stars. The total cross-section for the $^{6}Li$$\it{(p}$,$\alpha$)$^{3}He$ reaction has been measured before, in the proton energy range starting from 25 keV to several MeV. The so-called "Second Cosmological Lithium Problem" is concerned with the $^{6}Li$ isotope primordial abundance discrepancy. It states that the measured abundance exceeds the predictions of the Standard Big Bang Nucleosynthesis theory by several orders of magnitude.
The existing $^{6}Li$$\it{(p}$,$\alpha$)$^{3}He$ direct measurement data suffer from large uncertainty, particularly at energies below 500 keV (in the center-of-mass system). Thus, a new direct measurement of the $^{6}Li$$\it{(p}$,$\alpha$)$^{3}He$ reaction at low energies, from 122 keV to 1.2 MeV (4 different beam energies) in the center-of-mass system has been carried out to reduce the uncertainty in the S(E) factor. The scaled-down version of the ELISSA array having 12 X3 position-sensitive strip detectors arranged in a ring-like configuration was used to detect the reaction products. The total cross-sections of $^{6}Li$+p was obtained by fitting the angular distributions of the present data with CRC (couple reaction channel) calculations by using the FRESCO code. The S-factor was deduced from the total cross sections, and compared with the available compilations for $^{6}Li$$\it{(p}$,$\alpha$)$^{3}He$ reaction. The present measurement resulted the S-factor with better consistency and lesser uncertainty, which will contribute to explaining the BBN network calculations.