We present long-term optical and RXTE data of two X-ray binary pulsars in theSmall Magellanic Cloud, SXP46.6 and SXP6.85. The optical light curves of bothsources show substantial (~0.5-0.8 mag) changes over the time span of theobservations. While the optical data for SXP6.85 do not reveal any periodicbehaviour, by detrending the optical measurements for SXP46.6 we find anorbital period of ~137 days, consistent with results from the X-ray data. Thedetection of Type I X-ray outbursts from SXP46.6, combined with the fact thatwe also see optical outbursts at these times, implies that SXP46.6 is a highorbital eccentricity system. Using contemporaneous optical spectra of SXP46.6we find that the equivalent width of the H_alpha emission line changes overtime indicating that the size of the circumstellar disc varies. By studying thehistory of the colour variations for SXP6.85 we find that the source getsredder as it brightens which can also be attributed to changes in thecircumstellar disc. We do not find any correlation between the X-ray andoptical data for SXP6.85. The results for SXP6.85 suggest that it is a loweccentricity binary and that the optical modulations are due to the Bephenomenon.
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