Abstract. We present the photometric observations of 8 Algol-type eclipsing binary systems showing mass transfer activity to study the pulsations in their primary component. These are important targets for asteroseismology to explore their internal structure using pulsation frequencies. High-speed photometric observations of these stars were taken using three-channel fast photometer attached to the 1.04-m Sampurnanand telescope at ARIES during the year 2006-2008. We detect the delta-Scuti type pulsations in primary component of three binary systems viz. X Tri, RW Per and TV Cas. We do not find any new frequency in the known delta-Scuti systems like RZ Cas, AB Cas and AS Eri. Also delta-Scuti variability in the mass transfer systems RY Per and ST Per is not observed. We obtain an empirical relation between the orbital period and pulsation period of the primary. A longer orbital period of a binary component indicates a longer pulsation period. It is also found that larger force F (exerted by the secondary onto one gram of the primary) gives small pulsation period. However, the empirical relation discussed here needs more theoretical and observational confirmations.