  The increasing sensitivity of instruments at X-ray and TeV energies have
revealed a large number of nebulae associated with bright pulsars. Despite this
large data set, the observed pulsar wind nebulae (PWNe) do not show a uniform
behavior and the main parameters driving features like luminosity,
magnetization, and others are still not fully understood. To evaluate the
possible existence of common evolutive trends and to link the characteristics
of the nebula emission with those of the powering pulsar, we selected a sub-set
of 10 TeV detections which are likely ascribed to young PWNe and model the
spectral energy distribution with a time-dependent description of the nebulae's
electron population. In 9 of these cases, a detailed PWNe model, using
up-to-date multiwavelength information, is presented. The best-fit parameters
of these nebula are discussed, together with the pulsar characteristics. We
conclude that TeV PWNe are particle-dominated objects with large
multiplicities, in general far from magnetic equipartition, and that relatively
large photon field enhancements are required to explain the high level of
Comptonized photons observed. We do not find significant correlations between
the efficiencies of emission at different frequencies and the magnetization.
The injection parameters do not appear to be particularly correlated with the
pulsar properties either. We find that a normalized comparison of the SEDs
(e.g., with the corresponding spin-down flux) at the same age significantly
reduces the spectral distributions dispersion.
