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When a pulsar is moving through a partially ionized medium, a fraction ofneutral Hydrogen atoms penetrate inside the pulsar wind and can bephoto-ionized by the nebula UV radiation. The resulting protons remainsattached to the magnetic field of the light leptonic pulsar wind enhancing itsinertia and changing the flow dynamics of the wind. We present here the firstnumerical simulations of such effect in the tails of bow shock nebulae. Weproduce a set of different models representative of pulsars moving in theinterstellar medium with different velocities, from highly subsonic tosupersonic, by means of 2D hydrodynamic relativistic simulations. We comparethe different tail morphologies with results from theoretical models of massloading in bow shocks. As predicted by analytical models we observe a fastsideways expansion of the tail with the formation of secondary shocks in theISM. This effect could be at the origin of the head-and-shoulder morphologyobserved in many BSPWNe.

Numerical simulations of mass loading in the tails of Bow Shock Pulsar Wind Nebulae