The relation between optical and X-ray flux variations of the black-hole candidate LMC X-3

Details The relation between optical and X-ray flux variations of the black-hole candidate LMC X-3 The relation between optical and X-ray flux variations of the black-hole candidate LMC X-3

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...184..201v&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 184, no. 1-2, Oct. 1987, p. 201-208.

Astronomy and Astrophysics

Astronomy

18

Black Holes (Astronomy), Light Curve, Magellanic Clouds, Variable Stars, X Ray Binaries, X Ray Spectra, Radial Velocity, Stellar Luminosity

Scientific paper

The authors present the results of V-band photometry of the optical counterpart of the black-hole candidate LMC X-3. The observations were made during a three-week period in December 1984, using CCD cameras at the Danish 1.5 m, and MPI 2.2 m telescopes at ESO, and the 1.0 m telescope at SAAO. In addition to an orbital brightness modulation of 0.15 mag LMC X-3 showed a secular brightness increase of ≡0.3 mag. Evidence is found that either the non-orbital variations are not smooth on a time scale of days, or the shape of the orbital light curve is not constant (or both). During the period of the optical observations LMC X-3 was observed five times with EXOSAT. The long-term optical brightness variation is correlated with the X-ray flux. If the X-ray flux does not show orbital variations, the observed long-term correlated X-ray/optical brightness variations of LMC X-3 can be described by a model comprising a constant secondary star, with V ≡ 17.5 and B-V ≡ -0.20, and a rather cool (T < 15,000K) accretion disk of variable brightness, radiating through reprocessing of X rays.

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