The eclipsing binary AI Phoenicis - New results based on an improved light curve analysis program

Abstract

The 24.6 day eclipsing binary AI Phe contains two sharp-lined stars of comparable luminosity which undergo total eclipse, and yet are well separated. Radial velocity, photometric, and ultraviolet observations of this star have been remodeled using our improved version of the Wilson-Devinney code on the University of Calgary's Cyber 205 and Myrias SPS-2 computers. This version now has a new atmospheres option which makes use of Kurucz' model atmospheres to approximate the surface fluxes of the two stars. With the option, light curve fitting is now demonstrably improved for optical wavelengths. Rough empirical corrections result in still further improvement, with smaller discrepancies in U and u than are found using either the blackbody approximation or the previously used (Carbon-Gingerich) atmospheres option. For a specified temperature, wavelength, and logg, interpolation is performed within a table of values representing the ratio of blackbody to stellar atmosphere flux. The model atmosphere option simulates fluxes in Strömgren uvby or Johnson UAEK bandpasses, as well as in other bandpasses with widths A log X = 0.1 in the range 0.316 to 3.550 pm, and A log X = 0.05 in the UV (at 10 specified wavelengths from 0.100 to 0.282 ^m). The limb darkening of the hotter component in the far UY as it undergoes total eclipse is also investigated and compared with Kurucz models.

Asiago eclipsing binaries program IV. SZ Camelopardalis, aβ Cephei pulsator in a quadruple, eclipsing system

“…A photometric solution for SZ Cam was obtained with the WD code (Wilson & Devinney 1971;Wilson 1998) in its WD98K93d version as developed by Milone et al (1992), by adopting the MODE-2 option, appropriate for detached binary stars, which implements Roche geometry and a detailed treatment of reflection and other physical phenomena. It adopted the mass ratio as provided by the spectral disentangling.…”

Fundamental Properties and Distances of Large Magellanic Cloud Eclipsing Binaries. IV. HV 5936

“…The fits to the light curves were carried out using an improved version of the Wilson-Devinney (W-D) program (Wilson & Devinney 1971) that includes a model atmosphere routine developed by Milone, Stagg, & Kurucz (1992) for the computation of the stellar radiative parameters. Both detailed reflection-model (MREF = 2, NREF = 1) and proximity-effect corrections were taken into account when fitting the light curves.…”

Detached binaries in the Large Magellanic Cloud

“…Stars are arranged according to the decreasing V magnitude. Milone et al (1992). The program is composed of the LC program generating light curves for assumed parameters and the differential correction program, DC.…”