Phenomenological modelling of light curves of non-eclipsing double stars

The brightness of close non-eclipsing binary systems and eclipsing binaries besides eclipses themselves is changing due to proximity effects which are the result of the mutual interaction between components. Although the shape of resulting light curves or their segments is smooth and rather simple, the physics of proximity effects, including the deformation of components caused by tides and mutual warming and illumination, is considerably complex and untransparent. It represents one of the chief reasons that the solution of close binary star light curve modelling is a tedious process. That is why we are aiming at the building of the pertinent phenomenological light curve models that are much swifter and more flexible than the physical ones. Using our new phenomenological model we are now able to fit light curves of non-eclipsing binary simulated by the most advanced physical binary model software as a Roche or Phoebe with the accuracy of 0.0003 mag. The phenomenological model can be applied for binaries with both the circular and the elliptical orbits. The model enables to determine the eccentricity and the orientation of the elliptical orbit of the binary; as well it is apt also for the analysis of the possible apsidal motion in such systems. Obtained phenomenological model of elliptical variables provides an effective instrument for distinguishing of their light curves from double-wave ones of magnetic chemical peculiar stars. The full paper will be published elsewhere soon.