  From data by LASCO C2 and C3 coronagraphs, depending on time (distance), we
have determined positions and velocities of the front for fast limb CMEs' body
with their sources near the limb, and for the body of halo-type CME with the
sources near the solar disk center. These characteristics of CME body are
compared to similar kinematic characteristics obtained for CME body-associated
shock waves (shocks). For the body of halo-type CME with the sources near the
solar disk center and associated shocks, we determined and compared their
kinematic characteristics in 3D space. It has been shown that for all the
considered CME groups, the shock velocity is higher than the CME body velocity,
both velocities decrease as the mass ejection moves. As this takes place, the
distance between CME body and shock grows. On average, distance from CME body
to shock, and velocity difference of these structures is greater for a halo
CME, and even greater for a model CME in 3D.
