  We present simultaneous, multi-wavelength observations of the Small
Magellanic Cloud Be/XRB IGR J01217-7257 (=SXP 2.16) during outbursts in 2014,
2015 and 2016. We also present the results of RXTE observations of the Small
Magellanic Cloud during which the source was initially discovered with a
periodicity of 2.1652$\pm$0.0001 seconds which we associate with the spin
period of the neutron star. A systematic temporal analysis of long term
Swift/BAT data reveals a periodic signal of 82.5$\pm$0.7 days, in contrast with
a similar analysis of long base line OGLE I-band light curves which reveals an
83.67$\pm$0.05 days also found in this work. Interpreting the longer X-ray
periodicity as indicative of binary motion of the neutron star, we find that
outbursts detected by INTEGRAL and Swift between 2014 and 2016 are consistent
with Type I outbursts seen in Be/XRBs, occurring around periastron. Comparing
these outbursts with the OGLE data, we see a clear correlation between outburst
occurrence and increasing I-band flux. A periodic analysis of subdivisions of
OGLE data reveals three epochs during which short periodicities of $\sim$1 day
are significantly detected which we suggest are non-radial pulsations (NRPs) of
the companion star. These seasons immediately precede those exhibiting clear
outburst behaviour, supporting the suggested association between the NRPs,
decretion disk growth and the onset of Type I outbursts.
