# Full-3D relativistic MHD simulations of Bow Shock Pulsar Wind Nebulae: dynamics

## TL;DR

This study uses 3D relativistic MHD simulations to explore how pulsar wind properties influence the diverse shapes and behaviors of bow shock pulsar wind nebulae, focusing on fluid structure, magnetic fields, and turbulence.

## Contribution

It provides a comprehensive analysis of how different pulsar wind injection conditions affect nebular dynamics and morphology in BSPWNe through detailed simulations.

## Key findings

- Variations in wind anisotropy and magnetization impact nebular shape.
- Turbulence levels correlate with injection parameters.
- Magnetic field structures and current sheet survival depend on wind properties.

## Abstract

Bow shock pulsar wind nebulae (BSPWNe) are know to show a large variety of shapes and morphologies, both when comparing different objects, and for the same object in different energy bands. It is unclear if such a variety is related to differences in the pulsar wind properties, or to differences in the conditions of the ambient medium. We present here a set of full three-dimensional, relativistic and magneto-hydrodynamic simulations of BSPWNe, with the intention of determining how differences in the injection conditions by the pulsar wind reflect in the nebular dynamics. To achieve a good coverage of the available parameter space we have run several simulations varying those parameters that are most representative of the wind properties: the latitudinal anisotropy of the wind energy flux with respect to the pulsar spin axis, the level of magnetization, the inclination of the pulsar spin axis with respect to the pulsar direction of motion. We have followed the dynamics in these systems, not just in the very head, but also in the tail, trying to assess if and how the system retains memory of the injection at large distances from the pulsar itself. In this paper we focus our attention on the characterization of the fluid structure and magnetic field properties. We have tried to evaluate the level of turbulence in the tail, and its relation to injection, the survival of current sheets, and the degree of mixing between the shocked ambient medium and the relativistic pulsar wind material.