  Spallative nucleosynthesis is thought to be the only process capable of
producing significant amount of Beryllium (Be) in the universe. Therefore, both
energetic particles (EPs) and nuclei to be spalled (most efficiently C, N and O
nuclei in this case) are required, which indicates that supernovae (SNe) may be
directly involved in the synthesis of the Be nuclei observed in the halo stars
of the Galaxy. We apply current knowledge relating to supernova remnant (SNR)
evolution and particle shock acceleration to calculate the total Be yield
associated with a SN explosion in the interstellar medium, focusing on the
first stages of Galactic chemical evolution (i.e. when metallicity Z < 0.01
Z_odot) We show that dynamical aspects must be taken into account carefully,
and present analytical calculations of the spallation reactions induced by the
EPs accelerated at both the forward and the reverse shocks following the SN
explosion. Our results show that the production of Be in the early Galaxy is
still poorly understood, and probably implies either selective acceleration
processes (greatly favouring CNO acceleration), reconsideration of the
observational data (notably the O vs. Fe correlation), or even new energy
sources.
