This paper presents analysis and interpretation of OGLE photometric data of four X-ray binary pulsar systems in the Small Magellanic Cloud : 1WGA J0054.9-7226 , RX J0050.7-7316 , RX J0049.1-7250 , and 1SAX J0103.2-7209 .
In each case , the probable optical counterpart is identified on the basis of its optical colours .
In the case of RX J0050.7-7316 the regular modulation of its optical light curve appears to reveal an ellipsoidal modulation with a period of 1.416 days .
Using reasonable masses for the neutron star and the B star , we show that the amplitude and relative depths of the minima of the I-band light curve of RX J0050.7-7316 can be matched with an ellipsoidal model where the B star nearly fills its Roche lobe .
For mass ratios in the range of 0.12 to 0.20 , the corresponding best-fitting inclinations are about 55 degrees or larger .
The neutron star would be eclipsed by the B star at inclinations larger than \approx 60 ^ { \circ } for this particular mass ratio range .
Thus RX J0050.7-7316 is a good candidate system for further study .
In particular , we would need additional photometry in several colours , and most importantly , radial velocity data for the B star before we could draw more quantitative conclusions about the component masses .