  Identification and characterization of a rapidly increasing number of pulsar
wind nebulae is, and will continue to be, a challenge of high-energy gamma-ray
astrophysics. Given that such systems constitute -- by far -- the most numerous
expected population in the TeV regime, such characterization is important not
only to learn about the sources per se from an individual and population
perspective, but also to be able to connect them with observations at other
frequencies, especially in radio and X-rays. Also, we need to remove the
emission from nebulae in highly confused regions of the sky for revealing other
underlying emitters. In this paper we present a new approach for theoretical
modelling of pulsar wind nebulae: a hybrid hydrodynamic-radiative model able to
reproduce morphological features and spectra of the sources, with relatively
limited numerical cost.
