  We explore the relationship among three coronal mass ejections (CMEs),
observed on 28 October 2003, 7 November 2004, and 20 January 2005, the type II
burst-associated shock waves in the corona and solar wind, as well as the
arrival of their related shock waves and magnetic clouds at 1 AU. Using six
different coronal/interplanetary density models, we calculate the speeds of
shocks from the frequency drifts observed in metric and decametric radio wave
data. We compare these speeds with the velocity of the CMEs as observed in the
plane-of-the-sky white-light observations and calculated with a cone model for
the 7 November 2004 event. We then follow the propagation of the ejecta using
Interplanetary Scintillation (IPS) measurements, which were available for the 7
November 2004 and 20 January 2005 events. Finally, we calculate the travel time
of the interplanetary (IP) shocks between the Sun and Earth and discuss the
velocities obtained from the different data. This study highlights the
difficulties in making velocity estimates that cover the full CME propagation
time.
