A Laminar Model for the Magnetic Field Structure in Bow-Shock Pulsar Wind Nebulae
arXiv:1805.01653 · doi:10.1093/mnras/sty1199
Abstract
Bow Shock Pulsar Wind Nebulae are a class of non-thermal sources, that form when the wind of a pulsar moving at supersonic speed interacts with the ambient medium, either the ISM or in a few cases the cold ejecta of the parent supernova. These systems have attracted attention in recent years, because they allow us to investigate the properties of the pulsar wind in a different environment from that of canonical Pulsar Wind Nebulae in Supernova Remnants. However, due to the complexity of the interaction, a full-fledged multidimensional analysis is still laking. We present here a simplified approach, based on Lagrangian tracers, to model the magnetic field structure in these systems, and use it to compute the magnetic field geometry, for various configurations in terms of relative orientation of the magnetic axis, pulsar speed and observer direction. Based on our solutions we have computed a set of radio emission maps, including polarization, to investigate the variety of possible appearances, and how the observed emission pattern can be used to constrain the orientation of the system, and the possible presence of turbulence.
13 pages, 12 figures, accepted for publication in MNRAS
References in corpus (26)
- Observation of an anomalous positron abundance in the cosmic radiation
- The observed velocity distribution of young pulsars
- Simulated synchrotron emission from Pulsar Wind Nebulae
- MAGMA: a 3D, Lagrangian magnetohydrodynamics code for merger applications
- Non-thermal emission from relativistic MHD simulations of PWNe: from synchrotron to inverse Compton
- Geminga's puzzling pulsar wind nebula
- Pulsar Wind Nebulae Created by Fast-Moving Pulsars
- Evidence for alignment of the rotation and velocity vectors in pulsars. II. Further data and emission heights
- X-ray Observations of Parsec-Scale Tails behind Two Middle-Aged Pulsars
- On the X-ray feature associated with the Guitar Nebula
- Dissipation of the striped pulsar wind
- Three-dimensional hydrodynamic simulations of asymmetric pulsar wind bow shocks
- X-ray emission properties of the old pulsar PSR B2224+65
- Constraints on particle acceleration sites in the Crab Nebula from relativistic MHD simulations
- Multi-D magnetohydrodynamic modelling of pulsar wind nebulae: recent progress and open questions
- Chaotic properties of a turbulent isotropic fluid
- Chandra observations of the pulsar PSR B1929+10 and its environment
- Deep Chandra Observations of the Pulsar Wind Nebula Created by PSR B0355+54
- Expansion measurement of Supernova Remnant RX J1713.7-3946
- Kinematics of the Galactic SNR G109.1-1.0 (CTB 109)
- Modeling the effect of small-scale magnetic turbulence on the X-ray properties of Pulsar Wind Nebulae
- Investigating CXOU J163802.6-471358: a new pulsar wind nebula in the Norma region?
- Modeling Pulsar Wind Nebulae
- Multidimensional relativistic MHD simulations of Pulsar Wind Nebulae: dynamics and emission
- Pulsar striped winds
- Modeling Radio Circular Polarization in the Crab Nebula
Cited by in corpus (8)
- Full-3D relativistic MHD simulations of Bow Shock Pulsar Wind Nebulae: dynamics
- Full-3D relativistic MHD simulations of bow shock pulsar wind nebulae: emission and polarization
- From young to old: the evolutionary path of Pulsar Wind Nebulae
- Escape of High Energy Particles from Bow-Shock Pulsar Wind Nebulae
- Evolved Pulsar Wind Nebulae
- 3D Relativistic MHD Simulations of Pulsar Bow Shock Nebulae
- Pulsar Wind Nebulae
- Resolving the bow shock and tail of the cannonball pulsar PSR J0002+6216