CCD photometry of variable stars in the Magellanic Clouds - VI. The eclipsing binary HV982 in the Large Magellanic Cloud

Details CCD photometry of variable stars in the Magellanic Clouds - VI. The eclipsing binary HV982 in the Large Magellanic Cloud CCD photometry of variable stars in the Magellanic Clouds - VI. The eclipsing binary HV982 in the Large Magellanic Cloud

Oct 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mnras.299.1087p&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 299, Issue 4, pp. 1087-1096.

Astronomy and Astrophysics

Astronomy

7

Binaries: Eclipsing, Stars: Early-Type, Stars: Fundamental Parameters, Stars: Individual: Hv982, Magellanic Clouds, Ultraviolet: Stars

Scientific paper

Using improved techniques, high-quality CCD uvbyVI photometry has been obtained for the eclipsing binary HV982 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+/-7yr. The effective temperatures of the components are found via flux fitting to be T_eff,1=28000+/-5000K and T_eff,2=27 200+/-5000K. The large errors result from uncertainties over the appropriate interstellar extinction correction. The system plausibly comprises two ~8M stars of radius 6-7R separated by ~30R. 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_gamma<10^-41kg. Because of the great distance to HV982, 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.

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