“…Short period close binaries (e.g., EP And) i.e., those having an orbital period P , 5À6 days, possess the above mentioned characteristics, due to rapid rotation (Richard & Albright 1993). Many authors (see e.g., Richards 1993Richards , 1992Hall 1989& Olson 1981 have discussed that the secondary and/or primary in the close binaries having a late type component show a variety of time dependent magnetic properties, which may cause, brightness variations in the LC (particularly at mid primary eclipse), radiations of X-ray, Ultraviolet, infrared, and cyclic variations in the orbital period of the binary (through a mechanism purposed by Applegate 1992 and modified by Lanza et al 1998& Lanza 2005. This mechanism is based on the variation of the active star shape through a change in the Gravitational Quadrupole Moment (GQM) of the star.…”