We investigate energetic type Ic supernovae as production sites for ^ { 6 } Li and Be in the early stages of the Milky Way .
Recent observations have revealed that some very metal-poor stars with [ Fe/H ] < -2.5 possess unexpectedly high abundances of ^ { 6 } Li .
Some also exbihit enhanced abundances of Be as well as N. From a theoretical point of view , recent studies of the evolution of metal-poor massive stars show that rotation-induced mixing can enrich the outer H and He layers with C , N , and O ( CNO ) elements , particularly N , and at the same time cause intense mass loss of these layers .
Here we consider energetic supernova explosions occurring after the progeniter star has lost all but a small fraction of the He layer .
The fastest portion of the supernova ejecta can interact directly with the circumstellar matter ( CSM ) , both composed of He and CNO , and induce light element production through spallation and He-He fusion reactions .
The CSM should be sufficiently thick to energetic particles so that the interactions terminate within its innermost regions .
We calculate the resulting ^ { 6 } Li/O and ^ { 9 } Be/O ratios in the ejecta + CSM material out of which the very metal-poor stars may form .
We find that they are consistent with the observed values if the mass of the He layer remaining on the pre-explosion core is \sim 0.01 - 0.1 ~ { } M _ { \odot } , and the mass fraction of N mixed in the He layer is \sim 0.01 .
Further observations of ^ { 6 } Li , Be and N at low metallicity should provide critical tests of this production scenario .