Pulsar bow-shock nebulae. II. Hydrodynamical simulation

TL;DR

This paper presents hydrodynamical simulations of pulsar bow-shock nebulae, exploring the effects of magnetic fields and ISM interactions to better understand their observable properties and improve detection criteria.

Contribution

It introduces a 2-D hydrodynamical model including magnetic fields and compares results with analytical models to enhance understanding of pulsar bow-shock nebulae.

Findings

Magnetic fields influence nebula shape and brightness.

Opacity estimates affect observable properties.

Simulation results align with analytical models.

Abstract

We present hydrodynamical simulations, using a 2-D two component model (ambient medium and pul sar wind have different specific heat ratios), of bow shocks in a representative regime for pu lsar wind driven bow-shock nebulae. We also investigate the behaviour of a passive toroidal ma gnetic field wound around the pulsar velocity direction. Moreover we estimate the opacity of t he bow-shock to penetration of ISM neutral hydrogen: this quantity affects observable properti es of the nebula, like its size, shape, velocity and surface brightness distribution. Finally we compare these numerical results with those from an analytical model. The development of mor e realistic models is needed in order to tune the criteria for searches of new such objects, a s well as to interpret data on the known objects.