  In this Letter, we study the kinematic properties of ascending hot blobs
associated with confined flares. Taking advantage of high-cadence
extreme-ultraviolet images provided by the Atmospheric Imaging Assembly on
board the Solar Dynamics Observatory, we find that for the 26 events selected
here, the hot blobs are first impulsively accelerated outward, but then quickly
slow down to motionlessness. Their velocity evolution is basically synchronous
with the temporal variation of the Geostationary Operational Environmental
Satellite soft X-ray flux of the associated flares, except that the velocity
peak precedes the soft X-ray peak by minutes. Moreover, the duration of the
acceleration phase of the erupting blobs is moderately correlated with that of
the flare rise phase. For nine of the 26 cases, the erupting blobs even appear
minutes prior to the onset of the associated flares. Our results show that a
fraction of confined flares also involve the eruption of a magnetic flux rope,
which sometimes is formed and heated prior to the flare onset. We suggest that
the initiation and development of these confined flares are similar to that of
eruptive ones, and the main difference may lie in the background field
constraint, which is stronger for the former than for the latter.
