Recent studies based on multi-dimensional numerical simulations have suggested that the first generation stars are low-mass deficient and their initial mass function is likely to be top-heavy. Massive first stars are expected to affect the evolution of the surrounding medium through their UV radiation and supernova explosions. Both processes should influence subsequent star formation by changing the thermal and dynamic property of the ambient gas. Whether first supernovae can trigger subsequent star formation has already been discussed in order to explain the metal abundance pattern of the extremely metal-poor stars observed in our Galactic halo. In those studies, however, the masses of the progenitor stars (i.e., the first stars) have been a central issue under debate, and the characteristics of the next-generation stars so formed have been directed little attention. In this study, we reexamine the condition that the first supernova can trigger subsequent star formation, taking into account non-equilibrium chemistry, and try to estimate the typical masses of the next-generation stars.