The tables are in plain unformatted ASCII.
The tabulation is as follows:
inclination 30 (2.5) 90 degr
mass-ratio 0.05 (0.05) 1.0
degree of contact 0 (0.5) 1
All the calculations here are for the gravity brightening
exponent equal to von Zeipel's
(Teff ~ g1.0) at high
effective temperatures (32,000 K) in the Cousins I-band (as used by
OGLE). These calculations have an exploratory nature and are not meant
to be used for any particular system. The adopted bracketing
atmospheres (34,500 and 30,250 K) were characterized by relative fluxes
1.078 and 0.922 and by the linear limb darkening coeffecients 0.20 and
Of note are the following properties, which distinguish the results for hot contact systems from those for the solar-type (W UMa) case:
There are two tables for the hot systems:
coef 138278 bytes, 13 columns
7 characters wide
Each line contains the value of inclination (degr), mass-ratio, and eleven cosine coefficients a0 to a10 (in light units, not magnitudes!). There are three successive tables of the coeffecients for three values of the degree of contact: f=0 (inner), f=0.5, f=1 (outer).
depth of minima 43589 bytes, 4 columns
7 characters wide
Each line of the table contains the value of inclination (degr), mass-ratio, and the depth of both minima (in maximum light units), 1-l(00) and 1-l(1800), for eclipses of more- and less-massive components, respectively. Therefore, eg. to find the magnitude drop at the eclipse of the more massive component, do not use the depth tabulated here, but the light l(00), according to: m(0) = -2.5 log l(00). The division into three parts of the table, for the three values of the degree of contact, is the same as for "coef_hot".
Note: A very good representation of a light curve can be usually obtained by calculating the Fourier series: l=Sum(ai*cos(2*pi*i*phase), and then truncating the curved part of the secondary (occultation) eclipse at the level l(1800) using the tables of the depth of secondary minima 1-l(1800)).