  GRO J1744-28, commonly known as the `Bursting Pulsar', is a low mass X-ray
binary containing a neutron star and an evolved giant star. This system,
together with the Rapid Burster (MXB 1730-33), are the only two systems that
display the so-called Type II X-ray bursts. These type of bursts, which last
for 10s of seconds, are thought to be caused by viscous instabilities in the
disk; however the Type II bursts seen in GRO J1744-28 are qualitatively very
different from those seen in the archetypal Type II bursting source the Rapid
Burster. To understand these differences and to create a framework for future
study, we perform a study of all X-ray observations of all 3 known outbursts of
the Bursting Pulsar which contained Type II bursts, including a population
study of all Type II X-ray bursts seen by RXTE. We find that the bursts from
this source are best described in four distinct phenomena or `classes' and that
the characteristics of the bursts evolve in a predictable way. We compare our
results with what is known for the Rapid Burster and put out results in the
context of models that try to explain this phenomena.
