The supernova remnants (SNRs) are most convincing candidates for the acceleration of cosmic-rays. Together with the TeV gamma-ray detection by CANGAROO and HESS, it is now confirmed that at least some of the SNRs can actually accelerate electrons up to > 10 TeV. However, such studies have not provided direct information on ``protons'', which is the major component of cosmic-rays. Here we propose to measure spatial distribution of accelerated protons in the shell of RCW 86, and its association with the high energy (>10 TeV) electrons which emit synchrotron X-rays up to 50 keV. Large effective area and the good detection capability of Suzaku will be ideal tools for our scientific goal.