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Our Galaxy is filled with cosmic-ray particles and more than 98% of them areatomic nuclei. In order to clarify their origin and acceleration mechanism,chemical composition measurements of these cosmic rays with wide energycoverage play an important role. Imaging Atmospheric Cherenkov Telescope (IACT)arrays are designed to detect cosmic gamma-rays in the very-high-energy regime($\sim$TeV). Recently these systems proved to be capable of measuringcosmic-ray chemical composition in the sub-PeV region by capturing directCherenkov photons emitted by charged primary particles. Extensive air showerprofiles measured by IACTs also contain information about the primary particletype since the cross section of inelastic scattering in the air depends on theprimary mass number. The Cherenkov Telescope Array (CTA) is the next generationIACT system, which will consist of multiple types of telescopes and have akm$^2$-scale footprint and extended energy coverage (20 GeV to 300 TeV). Inorder to estimate CTA potential for cosmic ray composition measurement, a fullMonte Carlo simulation including a description of extensive air shower anddetector response is needed. We generated a number of cosmic-ray nuclei events(8 types selected from H to Fe) for a specific CTA layout candidate in thesouthern-hemisphere site. We applied Direct Cherenkov event selection andshower profile analysis to these data and preliminary results on charge numberresolution and expected event count rate for these cosmic-ray nuclei arepresented.

A Monte Carlo simulation study for cosmic-ray chemical composition measurement with Cherenkov Telescope Array