Precision study of cosmic nuclei provides detail knowledge on the origin and propagation of cosmic rays. In the past, results of different experiments often had large uncertainty and are different of each other. AMS was designed to measure and identify cosmic ray nuclei with seven independent detectors, thus it is able to provide precision studies of nuclei simultaneously to multi-TeV energies. In 6 years on the Space Station, AMS has collected 100 billion both primary and secondary cosmic rays. Primary cosmic rays, such as p, He, C and O, are believed to be mainly produced and accelerated in supernova remnants, while secondary cosmic rays, such as Li, Be and B are thought to be produced by collisions of heavier nuclei with interstellar matter. The unique and distinct rigidity dependence of primary and secondary cosmic ray fluxes with charges Z=1 to Z=8 in the GV to TV rigidity range will be presented. The characteristics of the disagreement of the AMS results with the predictions of the GALPROP model will also be presented for each nuclei.