  We study the coronal mass ejection (CME) with a complex acceleration profile.
The event occurred on April 23, 2009. It had an impulsive acceleration phase,
an impulsive deceleration phase, and a second impulsive acceleration phase.
During its evolution, the CME showed signatures of different acceleration
mechanisms: kink instability, prominence drainage, flare reconnection, and a
CME-CME collision. The special feature of the observations is the usage of the
TESIS EUV telescope. The instrument could image the solar corona in the Fe 171
\AA\ line up to a distance of 2 $R_\odot$ from the center of the Sun. This
allows us to trace the CME up to the LASCO/C2 field of view without losing the
CME from sight. The onset of the CME was caused by kink instability. The mass
drainage occurred after the kink instability. The mass drainage played only an
auxiliary role: it decreased the CME mass, which helped to accelerate the CME.
The first impulsive acceleration phase was caused by the flare reconnection. We
observed the two ribbon flare and an increase of the soft X-ray flux during the
first impulsive acceleration phase. The impulsive deceleration and the second
impulsive acceleration phases were caused by the CME-CME collision. The studied
event shows that CMEs are complex phenomena that cannot be explained with only
one acceleration mechanism. We should seek a combination of different
mechanisms that accelerate CMEs at different stages of their evolution.
