2004MNRAS.349..833B

Using improved techniques, we have obtained CCD uV_JI_Cphotometry for three eclipsing binary stars in the Magellanic Clouds and made preliminary analyses of the light curves. MACHO*05:36:48.7-69:17:00 in the Large Magellanic Cloud (LMC) is a detached, eccentric system. Apsidal motion is detected with a period of 100±5 yr. The radii of the component stars are less than a fifth of their orbital separation and their masses are plausibly ∼14 and ∼20 M_☉. Similar masses may also characterize the components of MOA J005018.4-723855 in the Small Magellanic Cloud (SMC), but here the more massive star is cooler, fills its Roche lobe, and is probably in an early stage of case A mass transfer. MOA J005623.5-722123 in the SMC is detached with a nearly edge-on orbit. The masses are plausibly ∼14 and ∼16 M_☉. Because of polar gravity brightening, the star occulted at the shallower eclipse may actually have the higher mean effective temperature by a marginal amount.