The two CCD photometries of the intermediate polar TV Columbae are made for obtaining the two updated eclipse timings with high precision .
There is an interval time \sim 17 yr since the last mid-eclipse time observed in 1991 .
Thus , the new mid-eclipse times can offer an opportunity to check the previous orbital ephemerides .
A calculation indicates that the orbital ephemeris derived by ( 2 ) should be corrected .
Based on the proper linear ephemeris ( 9 ) , the new orbital period analysis suggests a cyclical period variation in the O-C diagram of TV Columbae .
Using Applegate ’ s mechanism to explain the periodic oscillation in O-C diagram , the required energy is larger than that a M0-type star can afford over a complete variation period \sim 31.0 ( \pm 3.0 ) yr .
Thus , the light travel-time effect indicates that the tertiary component in TV Columbae may be a dwarf with a low mass , which is near the mass lower limit \sim 0.08 M _ { \odot } as long as the inclination of the third body high enough .