The distances, central star parameters Tef , log g, L∗, M∗, and optical thicknesses of the envelopes in the Lyman limits of hydrogen and helium are determined in a self-consistent way for 156 planetary nebulae (PNe) in our Galaxy (129, 22, and 5 PNe in the galactic disk, bulge, and halo respectively). For each nebula, the distance is adjusted in such a way that the theoretical evolutionary age of the central star (CS) should be equal to the dynamical age of the expanding nebular envelope (Malkov, 1994). This method combines the individual approach to each nebula with the possibility of application to a large sample of PNe. Some improvements have been introduced in the method as compared with its original version. The evolutionary tracks and time scales for CS with masses of 0.605, 0.696, 0.836, and 0.940 M⊙ were taken from Blöcker (1995). The change of the nebular expansion velocity during the evolution of a PN was roughly taken into account. The effective temperature of the CS and related parameters were found by the generalized energy balance method (Malkov et al., 1995) or, in appropriate cases, by Zanstra methods. Observational data have been collected from 93 papers published in 1975–1995.