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Identification and characterization of a rapidly increasing number of pulsarwind nebulae is, and will continue to be, a challenge of high-energy gamma-rayastrophysics. Given that such systems constitute -- by far -- the most numerousexpected population in the TeV regime, such characterization is important notonly to learn about the sources per se from an individual and populationperspective, but also to be able to connect them with observations at otherfrequencies, especially in radio and X-rays. Also, we need to remove theemission from nebulae in highly confused regions of the sky for revealing otherunderlying emitters. In this paper we present a new approach for theoreticalmodelling of pulsar wind nebulae: a hybrid hydrodynamic-radiative model able toreproduce morphological features and spectra of the sources, with relativelylimited numerical cost.

Introducing the HD+B model for pulsar wind nebulae: a hybrid hydrodynamics/radiative approach