Three-dimensional relativistic MHD simulations of bow shock nebulae
Abstract
Bow shock pulsar wind nebulae have been observed with diverse morphologies, both when comparing the same source at different wavelengths or when looking at different objects. Different conditions of the surrounding medium or properties of the pulsar wind have been geneally invoked as possible causes of these diversities. Here we have investigated a large set of physical conditions of such systems by means of 3D relativistic MHD numerical simulations. A good coverage of the parameters space describing different conditions of the pulsar wind at injection is ensured with the variation of the most representative parameters: the level of magnetization, the latitudinal anisotropy of the wind energy flux, the inclination of the pulsar spin axis with respect to the star direction of motion. We have investigated the dynamics of the resulting bow shock nebulae and their tails, detailed the onset of turbulence and the effects on the emitting properties.
- Publication:
-
Memorie della Societa Astronomica Italiana
- Pub Date:
- 2020
- Bibcode:
- 2020MmSAI..91..260O
- Keywords:
-
- ISM: supernova remnants;
- ISM: cosmic rays;
- magnetic fields;
- MHD;
- methods: numerical;
- pulsars: general