Mkrtichian et al. (2002 Mkrtichian et al. ( , 2004 introduced a new class of semi-detached Algol-type systems which has mass-accreting pulsating primary components, so called oEA stars. The oEA stars generally lie inside the instability strip after the first high-mass transfer stage and the pulsational characteristics of primary components are similar to characteristics of classical δ Scuti type stars, while the evolutionary status of pulsating components is different. These stars are promising

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... targets for asteroseismic studies as their pulsation properties can be changed by the mass-accretion. Our report is a part of the "Thai Sky Survey for oEA Stars" (THASSOS) project initiated at the National Astronomical Institute of Thailand (NARIT) for detection of new oEA stars and studying their oscillation spectra. UW Vir is a semi-detached Algol-type eclipsing binary systems with P = 1.8107646 d orbital period. The coordinates are RA = 13 h 15 m 20. s 7355, DEC= −17 • 28 ′ 16. ′′ 924. The general properties of physical parameters in the binary system were determined by Brancewicz and Dworak (1980) . Qian (2000) studied the changes in orbital periods of UW Vir by O-C observations. The O-C curves represented the periodic variations superimposed on upward parabolic segments with periods of 45.9 years. The components of upward curving parabolic variations in UW Vir showed secular period increase with rates of +1.73 × 10 −6 d/yr respectively. The secular period increase in UW Vir indicated that the mass transfer occurs from the less to the more massive component which is consistent with their semi-detached configurations. In addition, the periodic changes of the orbital periods of UW Vir also caused by the light-time effects due to the existence of the third body. 12 nights of new photometric observation for UW Vir were acquired from 13 May Table 1: Pulsation frequencies and amplitudes.