UBV photometry of the optical candidate for LMC X-3

Details UBV photometry of the optical candidate for LMC X-3 UBV photometry of the optical candidate for LMC X-3

Oct 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...126..265v&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 126, no. 2, Oct. 1983, p. 265-268. Research supported by the Nederlandse Organ

Astronomy and Astrophysics

Astrophysics

18

Astronomical Photometry, Binary Stars, Magellanic Clouds, Ubv Spectra, Variable Stars, X Ray Sources, Brightness Distribution, Light Curve

Scientific paper

Results are reported of two weeks of optical photometry of the optical counterpart of LMC X-3 obtained in December 1981. When folded modulo the 1.7-d period recently proposed for this system on the basis of radial-velocity measurements, the data show a brightness minimum near the inferior conjunction of the X-ray source. Combining these data with photometry obtained in 1974, long-term brightness variations over a range of up to 0.5 mag are found. Removing these, a double-wave orbital light curve with an amplitude of about 0.2 mag is found. A mean period for the interval 1974-1981 of 1.70502 + or - 0.00005 d is determined. It is shown that the observed light curve may be dominated by ellipsoidal variations, and that an additional light source, presumably an accretion disk, is likely to be present in the system.

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