Detailed kinematic observations of the bright inner portion of the planetary nebula NGC 6543 are presented. These data, combined with imaging observations reported by Balick et al. (1987), show that the kinematics of the nebula are just as peculiar as its morphology. Empirically, it is found that a double bipolar model readily incorporates most observational information regarding the complex structure and kinematics of NGC 6543. It is proposed that fast winds from the central star of NGC 6543 interact hydrodynamically with the denser red giant envelope expelled earlier, as suggested by Kwok (1982) and others.