  The neutrino process ($\nu$-process) for the production of 7Li and 11B in
core-collapse supernovae (SNe) is extensively investigated. Initial abundances
of s-nuclei and other physical conditions are derived from an updated
calculation of the SN 1987A progenitor. The nuclear reaction network including
neutrino reactions is constructed with the variable order Bader-Deuflhard
integration method. We find that yields of 7Li and 11B significantly depend on
the stellar metallicity while they are independent of the weak s-process during
the stellar evolution. When the metallicity is high, there are more neutron
absorbers, i.e., 56Fe, 14N (from initial CNO nuclei), and 54Fe, and the neutron
abundance is small during the $\nu$-process. Since 7Be is predominantly
destroyed via 7Be(n,p)7Li, a change in the neutron abundance results in
different 7Be yields. Then, the calculated yield ratio 7Li/11B=0.93 for the
solar metallicity is larger than that for the SN 1987A 7Li/11B=0.80 by 16 % in
the inverted mass hierarchy case. We analyze contributions of respective
reactions as well as abundance evolution, and clarify the $\nu$-process of 7Li
and 11B.
