  Observations of the chemical and isotopic composition of light cosmic-ray
nuclei can be used to constrain the astrophysical models of cosmic-ray
transport and interactions in the Galaxy. Nearly 200,000 light nuclei (Z>2)
have been observed by AMS-01 during the 10-day flight STS-91 in June 1998.
Using these data, we have measured the relative abundance of light nuclei Li,
Be, B and C in the kinetic energy range 0.35 - 45 GeV/nucleon.
