scholarly journals A laminar model for the magnetic field structure in bow-shock pulsar wind nebulae

2018 ◽  
Vol 478 (2) ◽  
pp. 2074-2085 ◽  
Author(s):  
N Bucciantini
Keyword(s):  
Magnetic Field ◽  
Field Structure ◽  
Bow Shock ◽  
Pulsar Wind Nebulae ◽  
Magnetic Field Structure ◽  
Pulsar Wind ◽  
The Magnetic Field ◽  
Laminar Model

The Boomerang PWN G106.6+2.9 and the Magnetic Field Structure in Pulsar Wind Nebulae

2006 ◽  
Vol 638 (1) ◽  
pp. 225-233 ◽  
Author(s):  
Roland Kothes ◽  
Wolfgang Reich ◽  
Bulent Uyanıker
Keyword(s):  
Magnetic Field ◽  
Field Structure ◽  
Pulsar Wind Nebulae ◽  
Magnetic Field Structure ◽  
Pulsar Wind ◽  
The Magnetic Field

scholarly journals On the origin of jet-like features in bow shock pulsar wind nebulae

2019 ◽  
Vol 490 (3) ◽  
pp. 3608-3615 ◽  
Author(s):  
B Olmi ◽  
N Bucciantini
Keyword(s):  
Supernova Remnant ◽  
High Energy ◽  
Field Structure ◽  
Bow Shock ◽  
Pulsar Wind Nebulae ◽  
Magnetic Field Structure ◽  
X Ray ◽  
Class A ◽  
Pulsar Wind ◽  
High Energy Particles

ABSTRACT Bow shock pulsar wind nebulae are a large class of non-thermal synchrotron sources associated to old pulsars that have emerged from their parent supernova remnant and are directly interacting with the interstellar medium. Within this class a few objects show extended X-ray features, generally referred as ‘jets’, that defies all the expectations from the canonical MHD models, being strongly misaligned respect to the pulsar direction of motion. It has been suggested that these jets might originate from high energy particles that escape from the system. Here we investigate this possibility, computing particle trajectories on top of a 3D relativistic MHD model of the flow and magnetic field structure, and we show not only that beamed escape is possible, but that it can easily be asymmetric and charge separated, which as we will discuss are important aspects to explain known objects.

scholarly journals The Magnetic Be Star Sigma Orionis E

1987 ◽  
Vol 92 ◽  
pp. 82-83 ◽  
Author(s):  
C. T. Bolton ◽  
A. W. Fullerton ◽  
D. Bohlender ◽  
J. D. Landstreet ◽  
D. R. Gies
Keyword(s):  
Magnetic Field ◽  
Field Structure ◽  
High Signal ◽  
Rotational Period ◽  
Magnetic Field Structure ◽  
The Past ◽  
Distribution Of Elements ◽  
Be Star ◽  
Hα Emission ◽  
The Magnetic Field

Over the past two years, we have obtained high resolution high signal/noise (S/N) spectra of the magnetic Be star σ Ori E at the Canada-France-Hawaii Telescope and McDonald Observatory. These spectra, which cover the spectral regions 399-417.5 and 440-458.5 nm and the Hα line and have typical S/N>200 and spectral resolution ≃0.02 nm, were obtained at a variety of rotational phases in order to study the magnetic field structure, the distribution of elements in the photosphere, and the effects of the magnetic field on the emission envelope. Our analysis of these spectra confirms, refines and extends the results obtained by Landstreet & Borra (1978), Groote & Hunger (1982 and references therein), and Nakajima (1985).The Hα emission is usually double-peaked, but it undergoes remarkable variations with the 1.19081 d rotational period of the star, which show that the emitting gas is localized into two regions which co-rotate with the star.

Effect of the magnetic field structure on the intensity of electron cyclotron emission from the plasma of the L-2M stellarator

2006 ◽  
Vol 32 (6) ◽  
pp. 461-474 ◽  
Author(s):  
D. K. Akulina ◽  
G. A. Gladkov ◽  
S. E. Grebenshchikov ◽  
O. I. Fedyanin ◽  
S. V. Shchepetov
Keyword(s):  
Magnetic Field ◽  
Field Structure ◽  
Electron Cyclotron ◽  
Electron Cyclotron Emission ◽  
Magnetic Field Structure ◽  
Cyclotron Emission ◽  
The Magnetic Field

scholarly journals Lepton-driven Nonresonant Streaming Instability

2021 ◽  
Vol 923 (2) ◽  
pp. 208
Author(s):  
Siddhartha Gupta ◽  
Damiano Caprioli ◽  
Colby C. Haggerty
Keyword(s):  
Magnetic Field ◽  
Laboratory Experiments ◽  
Magnetized Plasma ◽  
Ion Current ◽  
Pulsar Wind Nebulae ◽  
Particle In Cell ◽  
Streaming Instability ◽  
Electrons And Positrons ◽  
Pulsar Wind ◽  
The Magnetic Field

Abstract A strong super-Alfvénic drift of energetic particles (or cosmic rays) in a magnetized plasma can amplify the magnetic field significantly through nonresonant streaming instability (NRSI). While the traditional analysis is done for an ion current, here we use kinetic particle-in-cell simulations to study how the NRSI behaves when it is driven by electrons or by a mixture of electrons and positrons. In particular, we characterize the growth rate, spectrum, and helicity of the unstable modes, as well the level of the magnetic field at saturation. Our results are potentially relevant for several space/astrophysical environments (e.g., electron strahl in the solar wind, at oblique nonrelativistic shocks, around pulsar wind nebulae), and also in laboratory experiments.

Radio Flares and the Magnetic Field Structure in Gamma‐Ray Burst Outflows

2005 ◽  
Vol 625 (1) ◽  
pp. 263-270 ◽  
Author(s):  
Jonathan Granot ◽  
Gregory B. Taylor
Keyword(s):  
Magnetic Field ◽  
Gamma Ray ◽  
Field Structure ◽  
Gamma Ray Burst ◽  
Magnetic Field Structure ◽  
The Magnetic Field
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