### Tables for the paper "A Simple Description of Light Curves of W
UMa Systems", Slavek Rucinski (1993), PASP, 105, 1433

#### Read Me First

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

** Note: **
All the calculations here are for the gravity brightening
exponent equal to 1/3 of von Zeipel's
(T_{eff} ~ g^{0.32}) at solar
effective temperatures (5770 K) in V-band. The adopted bracketing
atmospheres (5900 and 5660 K) were characterized by relative fluxes
1.093 and 0.909 and by the linear limb darkening coeffecients 0.57 and
0.61.

Separate (unpublished,
available only here )
results for the radiative (von Zeipel) law
at 32,000 K give very similar values of the Fourier coefficients which
confirms that contact-binary light curves are dominated by geometrical
rather than atmospheric effects.

There are two tables for solar-type W UMa systems:

coef 138276 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).

depths of minima 43587 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(0^{0}) and 1-l(180^{0}), 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(0^{0}), according to:
m(0) = -2.5 log l(0^{0}). The division into three parts of the table,
for the three values of the degree of contact, is the same as for "coef".

** 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(180^{0}) using the tables of the depth of secondary
minima 1-l(180^{0})).