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In this paper we present the identification of two periodic X-ray signalscoming from the direction of the Small Magellanic Cloud (SMC). On detectionwith the Rossi X-ray Timing Explorer (RXTE), the 175.4s and 85.4s pulsationswere considered to originate from new Be/X-ray binary (BeXRB) pulsars withunknown locations. Using rapid follow-up INTEGRAL and XMM-Newton observations,we show the first pulsar (designated SXP175) to be coincident with a candidatehigh-mass X-ray binary (HMXB) in the northern bar region of the SMC undergoinga small Type II outburst. The orbital period (87d) and spectral class(B0-B0.5IIIe) of this system are determined and presented here for the firsttime. The second pulsar is shown not to be new at all, but is consistent withbeing SXP91.1 - a pulsar discovered at the very beginning of the 13 year longRXTE key monitoring programme of the SMC. Whilst it is theoretically possiblefor accreting neutron stars to change spin period so dramatically over such ashort time, the X-ray and optical data available for this source suggest thisspin-up is continuous during long phases of X-ray quiescence, where accretiondriven spin-up of the neutron star should be minimal.

Contrasting behaviour from two Be/X-ray binary pulsars: insights into differing neutron star accretion modes