Open AccessCCD photometry of variable stars in the Magellanic Clouds — VI. The eclipsing binary HV 982 in the Large Magellanic Cloud
Author(s) -
J. Pritchard,
William Tobin,
M. Clark,
E. F. Guinan
Publication year - 1998
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 - 10.1046/j.1365-8711.1998.01849.x
Subject(s) - physics , photometry (optics) , large magellanic cloud , astrophysics , astronomy , variable star , stars , small magellanic cloud , binary number , arithmetic , mathematics
Using improved techniques, high‐quality CCD uvbyVI photometry has been obtained for the eclipsing binary HV 982 in the Large Magellanic Cloud (LMC). International Ultraviolet Explorer ultraviolet spectrophotometry was also obtained. These data have been analysed using the Wilson–Devinney synthetic light‐curve code and Kurucz low‐metallicity model atmospheres as well as the EBOP code. The system is detached and the orbit is eccentric. Apsidal motion is detected with apsidal period 205 ± 7 yr. The effective temperatures of the components are found via flux fitting to be T eff,1 = 28 000 ± 5000 K and T eff,2 = 27 200 ± 5000 K. The large errors result from uncertainties over the appropriate interstellar extinction correction. The system plausibly comprises two ∼ 8 M stars of radius 6–7 R separated by ∼ 30 R. For pedagogical and historical interest, the near simultaneity of the eclipse minima at different wavelengths is used to constrain the constancy of the speed of light with wavelength and the mass of the photon, yielding m γ < 10 −41 kg. Because of the great distance to HV 982, this limit is some 10 2 times smaller than previously achieved with eclipse timings, but it is nevertheless 10 orders of magnitude less stringent than that which is provided by satellite measurements of planetary magnetic fields.