  The Cherenkov Telescope Array (CTA) is planned to serve as a ground-based
observatory for (very-)high-energy gamma-ray astronomy, open to a wide
astrophysics community, providing a deep insight into the non-thermal
high-energy universe. It foresees a factor of ~10 improvement in sensitivity
above 100 GeV, with substantially better angular and spectral resolutions and
wider field-of-view in comparison with currently operational experiments. The
CTA consortium is investigating the different physics cases for different
proposed array configurations and subsets. Pulsar Wind Nebulae (PWNe), the most
numerous VHE Galactic sources, and Supernova Remnants (SNRs), believed to be
the acceleration sites of the bulk of cosmic rays, will be two of the main
observation targets for CTA. In this contribution, the main scientific goals
regarding PWNe and SNRs are discussed, and quantitative examples of the
capability of CTA to achieve these objectives are presented.
