2002MNRAS.335..941M

Long-term variations are well-known in Be X-ray binaries, and are attributed to non-orbital changes in the structure of the Be circumstellar (equatorial) disc. However, the time-scales involved are so long (tens of days to years) that systematic studies have been very restricted. The ∼8-yr MACHO monitoring of the Large Magellanic Cloud (LMC) therefore presents an ideal opportunity to undertake such studies of Be X-ray systems that lie within the monitored fields. Here we present MACHO observations of two LMC Be X-ray transients, EXO 0531-66 and H 0544-665, the light curves of which show substantial (∼0.5 mag) long-term variations. However, our analysis shows little evidence for any periodic phenomena in the light curves of either source. We find an upper limit for detection of a short (1-100 d) periodicity in the V - and R -band light curves of EXO 0531-66 of 0.041 mag and 0.047 mag semi-amplitude, respectively. The upper limits for the V - and R -band data of H 0544-665 are 0.054 mag and 0.075 mag semi-amplitude, respectively. Both EXO 0531-66 and H 0544-665 become redder as they brighten, possibly due to variations in the structure of the equatorial disc around the Be star. Spectra of both sources show Hα emission; for EXO 0531-66 we find the emission varies over time, thereby confirming its optical identification.