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The morphology of young Pulsar Wind Nebulae (PWN) is largely determined bythe properties of the wind injected by the pulsar. We have used a recentparametrization of the wind obtained from Force Free Electrodynamicssimulations of pulsar magnetospheres to simulate nebulae for different sets ofpulsar parameters. We performed axisymmetric Relativistic Magnetohydrodynamicssimulations to test the morphology dependence of the nebula on the obliquity ofthe pulsar and on the magnetization of the pulsar wind. We compare thesesimulations to the morphology of the Vela and Crab PWN. We find that themorphology of Vela can be reproduced qualitatively if the pulsar obliquityangle is alpha ~45deg and the magnetization of the wind is high (sigma_0 ~3.0). A morphology similar to the one of the Crab Nebula is only obtained forlow magnetization simulations with alpha >~ 45deg. Interestingly, we find thatKelvin-Helmholtz instabilities produce small scale turbulences downstream ofthe reverse shock of the pulsar wind.

The imprint of pulsar parameters on the morphology of Pulsar Wind Nebulae