We searched for circumbinary planets orbiting NY Vir in historical eclipse times including our long-term CCD data . Sixty-eight times of minimum light with accuracies better than 10 s were used for the ephemeris computations . The best fit to those timings indicated that the orbital period of NY Vir has varied due to a combination of two sinusoids with periods of P _ { 3 } =8.2 yr and P _ { 4 } =27.0 yr and semi-amplitudes of K _ { 3 } =6.9 s and K _ { 4 } =27.3 s , respectively . The periodic variations most likely arise from a pair of light-time effects due to the presence of third and fourth bodies that are gravitationally bound to the eclipsing pair . We have derived the orbital parameters and the minimum masses , M _ { 3 } \sin i _ { 3 } = 2.8 M _ { Jup } and M _ { 4 } \sin i _ { 4 } = 4.5 M _ { Jup } , of both objects . A dynamical analysis suggests that the outer companion is less likely to orbit the binary on a circular orbit . Instead we show that future timing data might push its eccentricity to moderate values for which the system exhibits long-term stability . The results demonstrate that NY Vir is probably a star-planet system , which consists of a very close binary star and two giant planets . The period ratio P _ { 3 } / P _ { 4 } suggests that a long-term gravitational interaction between them would result in capture into a nearly 3:10 mean motion resonance . When the presence of the circumbinary planets is verified and understood more comprehensively , the formation and evolution of this planetary system should be advanced greatly .