  We present the observations of a blowout jet that experienced two distinct
ejection stages. The first stage started from the emergence of a small positive
magnetic polarity, which cancelled with the nearby negative magnetic field and
caused the rising of a mini-filament and its confining loops. This further
resulted in a small jet due to the magnetic reconnection between the rising
confining loops and the overlying open field. The second ejection stage was
mainly due to the successive removal of the confining field by the
reconnection. Thus that the filament erupted and the erupting cool filament
material directly combined with the hot jet originated form the reconnection
region and therefore formed the cool and hot components of the blowout jet.
During the two ejection stages, cool H{\alpha} jets are also observed cospatial
with their coronal counterparts, but their appearance times are earlier than
the hot coronal jets a few minutes. Therefore, the hot coronal jets are
possibly caused by the heating of the cool H{\alpha} jets, or the rising of the
reconnection height from chromosphere to the corona. The scenario that magnetic
reconnection occurred between the confining loops and the overlying open loops
are supported by many observational facts, including the bright patches on the
both sides of the mini-filament, hot plasma blobs along the jet body, and
periodic metric radio type III bursts at the very beginnings of the two stages.
The evolution and characteristics of these features manifest the detailed
non-linear process in the magnetic reconnection.
