scholarly journals Multidimensional Relativistic MHD Simulations of Pulsar Wind Nebulae: Dynamics and Emission

2017 ◽  
pp. 215-246 ◽  
Author(s):  
Luca Del Zanna ◽  
Barbara Olmi
Keyword(s):  
Pulsar Wind Nebulae ◽  
Mhd Simulations ◽  
Pulsar Wind

scholarly journals Spherically symmetric relativistic MHD simulations of pulsar wind nebulae in supernova remnants

2003 ◽  
Vol 405 (2) ◽  
pp. 617-626 ◽  
Author(s):  
N. Bucciantini ◽  
J. M. Blondin ◽  
L. Del Zanna ◽  
E. Amato
Keyword(s):  
Supernova Remnants ◽  
Spherically Symmetric ◽  
Pulsar Wind Nebulae ◽  
Mhd Simulations ◽  
Pulsar Wind

scholarly journals Full-3D relativistic MHD simulations of bow shock pulsar wind nebulae: emission and polarization

2019 ◽  
Vol 488 (4) ◽  
pp. 5690-5701 ◽  
Author(s):  
B Olmi ◽  
N Bucciantini
Keyword(s):  
Three Dimensional ◽  
Polarized Light ◽  
Bow Shock ◽  
Synchrotron Emission ◽  
Pulsar Wind Nebulae ◽  
Emission Pattern ◽  
Mhd Simulations ◽  
Pulsar Wind ◽  
Relativistic Magnetohydrodynamics ◽  
The Magnetic Field

ABSTRACT Bow shock pulsar wind nebulae are observed with a variety of complex morphologies at different wavelengths, most likely due to differences in the magnetic field strength and pulsar wind geometry. Here we present a detailed analysis, showing how these differences affect the observational properties in these systems, focusing on non-thermal synchrotron emission. By adopting different prescriptions for the local emissivity, on top of the magnetic and flow patterns taken from three-dimensional (3D) high-resolution numerical simulations in relativistic magnetohydrodynamics (MHD), and considering various viewing angles, we try to characterize the main features of the emission and polarization, to verify if and how these can be used to get information, or to put constraints, on known objects. We found, for example, that conditions leading to a strong development of the turbulence in the bow shock tail produce substantial differences in the emission pattern, especially in polarized light.

scholarly journals Introducing the HD+B model for pulsar wind nebulae: a hybrid hydrodynamics/radiative approach

2020 ◽  
Vol 494 (3) ◽  
pp. 4357-4370
Author(s):  
B Olmi ◽  
D F Torres
Keyword(s):  
Gamma Ray ◽  
High Energy ◽  
Theoretical Modelling ◽  
X Rays ◽  
Pulsar Wind Nebulae ◽  
New Approach ◽  
Energy Gamma ◽  
Radiative Model ◽  
Pulsar Wind

ABSTRACT Identification and characterization of a rapidly increasing number of pulsar wind nebulae is, and will continue to be, a challenge of high-energy gamma-ray astrophysics. Given that such systems constitute -by far- the most numerous expected population in the TeV regime, such characterization is important not only to learn about the sources per se from an individual and population perspective, but also to be able to connect them with observations at other frequencies, especially in radio and X-rays. Also, we need to remove the emission from nebulae in highly confused regions of the sky for revealing other underlying emitters. In this paper, we present a new approach for theoretical modelling of pulsar wind nebulae: a hybrid hydrodynamic-radiative model able to reproduce morphological features and spectra of the sources, with relatively limited numerical cost.

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