The eclipsing variable star AM Leo (BD +10• 2234 A) is a bright component (V = 9.1− 9.7 mag) of the visual binary system ADS 8024 (ρ = 11′′ .4, θ = 270 • ) (Hiller et al. 2004). The most comprehensive survey of the photometric observations of AM Leo were given in the studies of Hiller et al. (2004) and Albayrak et al. (2005a). Many authors noted temporal variations in the light curve of AM Leo. Along with the light curve variations, orbital variations have been observed too. Various hypotheses were proposed to explain this phenomenon. The most likely reason for the period change in AM Leo is now considered to be the presence of a third body in the system. This hypothesis was first suggested by Demircan & Derman (1992) The CCD observations data were reduced using the MaxImDL and Muniwin (http://cmunipack.sourceforge.net) packages. The minima time were computed by a parabola fitting method and averaged from all filters used during the night. Values of the moments of
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