出版社：SISSA, Scuola Internazionale Superiore di Studi Avanzati
摘要：The amount of 6Li detected in metal poor stars is unexpectedly large compared to Big-Bang Nucleosynthesis (BBN) predictions. The radiative capture reaction D(a, g)6Li with a Q-value of 1.474MeV is the main reaction for 6Li production at temperatures of 0.3×109 K. The BBN energy window goes from EBBN =30 keV up to 300 keV, but direct measurements do not exist below a center-of-mass energy of 650 keV. On the other hand, theoretical calculations for the S-factor differ by more than one order of magnitude. The LUNA (Laboratory for Underground Nuclear Astrophysics) setup below the Gran Sasso mountain offers measurement conditions with a reduction of the cosmic ray induced μ-flux by six orders of magnitude. Predictions show that the cross section of s(EBBN) 2×10−11 b can be measured with a proper setup using in-beam g-spectroscopy there. A cross section measurement currently has been started.
