scholarly journals Real beads on virtual strings: Charged particles on magnetic field lines

2012 ◽  
Vol 80 (11) ◽  
pp. 985-989
Author(s):  
Boris Breizman ◽  
Vladimir Khudik
Keyword(s):  
Magnetic Field ◽  
Charged Particles ◽  
Field Lines ◽  
Virtual Strings

Synchrotron Radiation Spectra

1972 ◽  
Vol 2 (3) ◽  
pp. 142-144 ◽  
Author(s):  
L. J. Gleeson ◽  
K. C. Westfold
Keyword(s):  
Magnetic Field ◽  
Synchrotron Radiation ◽  
Energy Distribution ◽  
Power Law ◽  
Uniform Magnetic Field ◽  
Charged Particles ◽  
Radiation Spectra ◽  
Field Lines

In this paper we give an account of the corrections that must be made to the formula for the emissivity ηf due to a power-law energy distribution of ultrarelativistic charged particles in a uniform magnetic field B0 in directions well away from the field lines when the effects of upper and lower cut-off values E2 and E1 in the energy distribution are not negligible.

Magnetic Field Aligned Potentials as an Acceleration Mechanism at Jupiter

2021 ◽  
Author(s):  
Dave Constable ◽  
Licia Ray ◽  
Sarah Badman ◽  
Chris Arridge ◽  
Chris Lorch ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Temporal Evolution ◽  
Charged Particles ◽  
Uniform Mesh ◽  
Time Varying ◽  
Potential Structure ◽  
Field Aligned Current ◽  
Field Lines ◽  
The Magnetic Field ◽  
Insight Into

<p>Since arriving at Jupiter, Juno has observed instances of field-aligned proton and electron beams, in both the upward and downward current regions. These field-aligned beams are identified by inverted-V structures in plasma data, which indicate the presence of potential structures aligned with the magnetic field. The direction, magnitude and location of these potential structures is important, as it affects the characteristics of any resultant field-aligned current. At high latitudes, Juno has observed potentials of 100’s of kV occurring in both directions. Charged particles that are accelerated into Jupiter’s atmosphere and precipitate can excite aurora; likewise, particles accelerated away from the planet can contribute to the population of the magnetosphere.</p> <p>Using a time-varying 1-D spatial, 2-D velocity space Vlasov code, we examine magnetic field lines which extend from Jupiter into the middle magnetosphere. By applying and varying a potential difference at the ionosphere, we can gain insight into the effect these have on the plasma population, the potential structure, and plasma densities along the field line. Utilising a non-uniform mesh, additional resolution is applied in regions where particle acceleration occurs, allowing the spatial and temporal evolution of the plasma to be examined. Here, we present new results from our model, constrained, and compared with recent Juno observations, and examining both the upward and downward current regions.</p>

scholarly journals 3D study of centrifugal acceleration in isotropic photon fields

2019 ◽  
Vol 28 (11) ◽  
pp. 1950141
Author(s):  
G. G. Bakhtadze ◽  
V. I. Berezhiani ◽  
Z. Osmanov
Keyword(s):  
Magnetic Field ◽  
Single Particle ◽  
Stable Equilibrium ◽  
Charged Particles ◽  
Relativistic Dynamics ◽  
Centrifugal Acceleration ◽  
Study Behavior ◽  
Field Lines ◽  
Particle Approach

In this paper, we study relativistic dynamics of charged particles corotating with prescribed trajectories, having the shape of dipolar magnetic field lines. In particular, we consider the role of the drag force caused by the photon field the forming of equilibrium positions of the charged particles. Alongside a single particle approach, we also study behavior of ensemble of particles in the context of stable positions. As we have shown, the together they create surfaces where particles are at stable equilibrium positions. In this paper, we examine these shapes and study parameters they depend on. It has been found that under certain conditions, there are two distinct surfaces with stable equilibrium positions.

scholarly journals New Radiation Formulae of Relativistic Electrons in Curved Magnetic Field Lines

2002 ◽  
Vol 199 ◽  
pp. 400-401
Author(s):  
Ya.M. Sobolev
Keyword(s):  
Magnetic Field ◽  
Charged Particles ◽  
Relativistic Electrons ◽  
Force Line ◽  
Radiation Mechanism ◽  
Field Lines

Radiation mechanism for relativistc charged particles spiraling along curved magnetic field is considered. Emission from many electron revolutions around force line is taken into account.

scholarly journals L-shell and energy dependence of magnetic mirror point of charged particles trapped in Earth’s magnetosphere

2020 ◽  
Vol 72 (1) ◽  
Author(s):  
Pankaj K. Soni ◽  
Bharati Kakad ◽  
Amar Kakad
Keyword(s):  
Magnetic Field ◽  
Charged Particles ◽  
Magnetic Mirror ◽  
Theoretical Expression ◽  
Neutral Atmosphere ◽  
Loss Cone ◽  
Field Lines ◽  
Mirror Point ◽  
The Magnetic Field ◽  
Shell Energy

Abstract In the Earth’s inner magnetosphere, there exist regions like plasmasphere, ring current, and radiation belts, where the population of charged particles trapped along the magnetic field lines is more. These particles keep performing gyration, bounce and drift motions until they enter the loss cone and get precipitated to the neutral atmosphere. Theoretically, the mirror point latitude of a particle performing bounce motion is decided only by its equatorial pitch angle. This theoretical manifestation is based on the conservation of the first adiabatic invariant, which assumes that the magnetic field varies slowly relative to the gyro-period and gyro-radius. However, the effects of gyro-motion cannot be neglected when gyro-period and gyro-radius are large. In such a scenario, the theoretically estimated mirror point latitudes of electrons are likely to be in agreement with the actual trajectories due to their small gyro-radius. Nevertheless, for protons and other heavier charged particles like oxygen, the gyro-radius is relatively large, and the actual latitude of the mirror point may not be the same as estimated from the theory. In this context, we have carried out test particle simulations and found that the L-shell, energy, and gyro-phase of the particles do affect their mirror points. Our simulations demonstrate that the existing theoretical expression sometimes overestimates or underestimates the magnetic mirror point latitude depending on the value of L-shell, energy and gyro-phase due to underlying guiding centre approximation. For heavier particles like proton and oxygen, the location of the mirror point obtained from the simulation deviates considerably (∼ 10°–16°) from their theoretical values when energy and L-shell of the particle are higher. Furthermore, the simulations show that the particles with lower equatorial pitch angles have their mirror points inside the high or mid-latitude ionosphere.

On the motion of charged particles in a sheared force-free magnetic field

2002 ◽  
Vol 67 (2-3) ◽  
pp. 215-221 ◽  
Author(s):  
G. E. VEKSTEIN ◽  
N. A. BOBROVA ◽  
S. V. BULANOV
Keyword(s):  
Magnetic Field ◽  
Spatial Scale ◽  
Single Particle ◽  
Charged Particles ◽  
Magnetic Confinement ◽  
Larmor Radius ◽  
Field Variation ◽  
Particle Trajectories ◽  
Field Lines ◽  
Actual Particle

This paper considers single-particle trajectories in a planar sheared force-free magnetic field. A specific feature of this magnetic configuration is the absence of both gradient and curvature magnetic drifts, as well as a diamagnetic force along field lines. Therefore, in the framework of the drift approximation, the motion of the particle guiding centre does not feel the magnetic field's non-uniformity. Here we discuss how the latter affects actual particle trajectories, making them quite different from simple circular gyromotion even when the Larmor radius is small. It is also shown how magnetic confinement ceases to work when the Larmor radius becomes comparable to the spatial scale of the field variation.

Cross field thermal transport in highly magnetized plasmas

1992 ◽  
Vol 437 (1899) ◽  
pp. 55-65 ◽  
Keyword(s):  
Magnetic Field ◽  
Heat Flux ◽  
Kinetic Equation ◽  
Mass Transport ◽  
Heat Transport ◽  
Electrostatic Interactions ◽  
Charged Particles ◽  
Non Local ◽  
Field Lines ◽  
The Magnetic Field

We construct a non-local kinetic equation for a plasma in a very strong magnetic field B where the charged particles coincide with their guiding centres and have zero drifts. It is shown that, although in this system mass transport occurs only along the field lines, heat transport cannot be confined only in the direction of the magnetic field. In particular, we estimate that a finite cross field heat flux scaling as 3/2 n ∂ T /∂ t = ∂( k ∞ ⊥ ∂ T /∂ x )∂ x ; k ∞ ⊥ = 3/2π ½ ( n 2 e 4 / m ½ T 3/2 ) L 2 ⊥ can be driven by collisions between like particles at the limit B → ∞. Hence, the classical B -2 dependence of k ⊥ must be modified to comply with this result. The choice of the cut-off length L ⊥ , representing the distance across B over which electrostatic interactions can be sustained, is discussed briefly at the end of the present work.

scholarly journals Persistent random walks of charged particles across magnetic field lines

2020 ◽  
Vol 102 (5) ◽  
Author(s):  
M. Baquero-Ruiz ◽  
A. Fasoli ◽  
I. Furno ◽  
F. Manke ◽  
P. Ricci
Keyword(s):  
Magnetic Field ◽  
Random Walks ◽  
Charged Particles ◽  
Persistent Random Walks ◽  
Field Lines

Particle Motions in Planetary Magnetic Fields: Europlanet Service

2020 ◽  
Author(s):  
Patrick Guio ◽  
Nicholas Achilleos ◽  
Nicolas André
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Charged Particles ◽  
High Energy ◽  
Particle Energy ◽  
Curvature Radius ◽  
High Energy Particle ◽  
Field Curvature ◽  
Planetary Magnetic Fields ◽  
Field Lines

<p>The trapping of charged particles in planetary magnetic fields is a process which underpins many important aspects of planetary magnetospheres, such as ring current evolution, particle acceleration, and the flow of current through the system, both free and bound. As part of our effort for the Europlanet project, the UCL group have developed codes which accurately model the trajectories of charged particles in magnetic field models appropriate for the magnetospheres of Jupiter and Saturn. These will form the basis of a service for the SPIDER task. In this presentation, we show examples of ion trajectories at both planets for representative 'start values' of equatorial distance, pitch angle, and values of particle energy. The simulations provide an indication of how particle orbits become less adiabatic as one approaches energies where gyroradii become comparable to magnetic field curvature radius. The disk-like fields of the gas giants are particularly effective at 'scattering' adequately high-energy particle trajectories as they cross the equator, where the field lines are most 'pinched' and have the smallest length scales.</p>

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