phase = 1.0000
Fig. 8.1 The limit of an eclipse of an over-contact system. Created with the help of BM2 (Bradstreet 1993)
toward the observer. The surface elements may be shown in both spherical and cylindrical coordinates. One of its most interesting features is the demonstration of the effects of star spot regions on the light and radial velocity curves and on the profiles.
The present version (3.0) at the time of this writing does not make use of the 1992 WD or WD93K93 program features such as asynchronous rotation, nonlinear limb-darkening, multiple reflection, or Kurucz atmosphere calculations. However,
most of the features available in the pre-1979 version of the WD program are included. Unlike BM2, however, eccentric orbits are treated and BM3 runs on a variety of platforms, including Windows on PCs, Unix, and Macintosh computers.
The program has many uses for both research and teaching. It is perhaps most valuable for demonstrating the effects on the synthetic light and radial velocity curves and profiles of changes of particular parameters. The manual has been updated and defines many of the classical WD program features. We cannot recommend it strongly enough; indeed, we have illustrated many of the useful features of Binary Maker 3.0 repeatedly throughout this book, just as the previous edition made use of BM2 illustrations.
In Figs. 8.1-8.3 we show some pictures produced with Binary Maker 2.0 showing the light curve, radial velocity curve, and three-dimensional shape of an eclipsing binary system. They were produced to determine, for predefined geometry, the smallest inclination which leads to an eclipse.
The following parameters have been used to produce the plots:
q = X [nm] T [K] g1 = g2 xt = x2 A1 = A2 I3 0.5 2.875 550 5500 0.32 0.6 0.5 0
The normalization phase has been set to 0.25 and the phase increment was 0.01. For the first four figures we used the latitude and longitude grid numbers 10 and 20, while for the last two figures we chose 15 and 30.
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