  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 60
degrees 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.
