The neutrino-nucleus reaction cross sections of super(4)He and super(12)C are evaluated using new shell model Hamiltonians. Branching ratios of various decay channels are calculated to evaluate the yields of Li, Be, and B produced through the v-process in supernova explosions. The new cross sections enhance the yields of super(7)Li and super(11 )B produced during the supernova explosion of a 16.2 M sub(image) star model compared to the case using the conventional cross sections by about 10%. On the other hand, the yield of super(10)B decreases by a factor of 2. The yields of super(6)Li, super(9)Be, and the radioactive nucleus super(10)Be are found at a level of image10 super(-11) M sub(image). The temperature of image - and image - neutrinos inferred from the supernova contribution of super( 11)B in Galactic chemical evolution models is constrained to the 4.3-6.5 MeV range. The increase in the super(7)Li and super(11)B yields due to neutrino oscillations is demonstrated with the new cross sections.