Open AccessCCD photometry of variable stars in the Magellanic Clouds – VII. The eclipsing binaries MACHO*05:36:48.7−69:17:00 in the LMC, and MOA J005018.4−723855 and J005623.5−722123 in the SMC
Author(s) -
Bayne G. P.,
Tobin W.,
Pritchard J. D.,
Pollard K. R.,
Albrow M. D.
Publication year - 2004
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2004.07535.x
Subject(s) - physics , astrophysics , photometry (optics) , large magellanic cloud , astronomy , roche lobe , stars , orbital period , light curve , small magellanic cloud , binary star
Using improved techniques, we have obtained CCD uV J I C photometry 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.