Charged Particles in Magnetic Fields

1989 ◽  
pp. 145-171 ◽  
Author(s):  
Walter Greiner
Keyword(s):  
Magnetic Fields ◽  
Charged Particles

ENERGY ORDERING EFFECTS IN THE ARRIVAL DIRECTIONS OF ULTRA-HIGH ENERGY COSMIC RAYS MEASURED BY THE PIERRE AUGER OBSERVATORY

2011 ◽  
Vol 20 (supp02) ◽  
pp. 50-56
Author(s):  
◽  
PETER SCHIFFER
Keyword(s):  
Cosmic Rays ◽  
Magnetic Fields ◽  
Charged Particles ◽  
High Energy ◽  
Pierre Auger Observatory ◽  
Ultra High Energy ◽  
High Energy Cosmic Rays ◽  
Ordering Effects ◽  
Arrival Directions

The Pierre Auger Observatory is the world's largest experiment for the measurement of ultra-high energy cosmic rays (UHECRs). These UHECRs are assumed to be to be charged particles, and thus are deflected in cosmic magnetic fields. Recent results of the Pierre Auger Observatory addressing the complex of energy ordering of the UHECRs arrival directions are reviewed in this contribution. So far no significant energy ordering has been observed.

Ion acceleration by multiple laser pulses and their spontaneous electromagnetic fields in plasma

2008 ◽  
Vol 74 (1) ◽  
pp. 111-118
Author(s):  
FEN-CE CHEN
Keyword(s):  
Magnetic Fields ◽  
Electric Field ◽  
Analytical Model ◽  
Electromagnetic Fields ◽  
Equations Of Motion ◽  
Charged Particles ◽  
Laser Pulses ◽  
The Self ◽  
Electric And Magnetic Fields ◽  
Relativistic Equations

AbstractThe acceleration of ions by multiple laser pulses and their spontaneously generated electric and magnetic fields is investigated by using an analytical model for the latter. The relativistic equations of motion of test charged particles are solved numerically. It is found that the self-generated axial electric field plays an important role in the acceleration, and the energy of heavy test ions can reach several gigaelectronvolts.

Gas-filled detectors

2020 ◽  
pp. 171-254
Author(s):  
Hermann Kolanoski ◽  
Norbert Wermes
Keyword(s):  
Magnetic Fields ◽  
Particle Physics ◽  
Parallel Plate ◽  
Charged Particles ◽  
Aging Effects ◽  
Charge Generation ◽  
Detector Performance ◽  
Time Projection Chambers ◽  
Drift Chambers ◽  
Time Projection

Detectors that record charged particles through their ionisation of gases are found in many experiments of nuclear and particle physics. By conversion of the charges created along a track into electrical signals, particle trajectories can be measured with these detectors in large volumes, also inside magnetic fields. The operation principles of gaseous detectors are explained, which include charge generation, gas amplification, operation modes and gas mixtures. Different detector types are described in some detail, starting with ionisation chambers without gas amplification, proceeding to those with gas amplification like spark and streamer chambers, parallel plate arrangements, multi-wire proportional chambers, chambers with microstructured electrodes, drift chambers, and ending with time-projection chambers. The chapter closes with an overview of aging effects in gaseous detectors which cause negative alterations of the detector performance.

scholarly journals The Magnetic Fields of Pulsars

1974 ◽  
Vol 64 ◽  
pp. 187-187
Author(s):  
D. M. Sedrakian
Keyword(s):  
Magnetic Field ◽  
Angular Velocity ◽  
Magnetic Fields ◽  
Relative Motion ◽  
Kinematic Viscosity ◽  
Charged Particles ◽  
Normal Fluid ◽  
Inertia Effects ◽  
Generation Mechanisms ◽  
Image Position

Two generation mechanisms of magnetic fields in pulsars are considered.If the temperature of a star is more than 108K, the star consists of a normal fluid of neutrons, protons and electrons. Because the angular velocity of pulsars is not constant dω/dt ≠0, inertia effects can occur, and generate magnetic fields through the relative motion of charged particles with different masses. The kinematic viscosity of electrons is 30 times larger than that of protons; hence electrons move with the crust, but the proton-neutron fluid will move relative to the electrons. The magnetic momentum can be calculated by the following formula where Meff = Mp + Mn(Nn/Np), R = radius of the star, σ = conductivity. For typical neutron stars we have dω/dt~ 10-8 s-2, R~106 cm, σ~1029 s-1 and we get a magnetic field of the order of 1010 G.

scholarly journals 12. Solar electrodynamics

1958 ◽  
Vol 6 ◽  
pp. 105-113 ◽  
Author(s):  
T. G. Cowling
Keyword(s):  
Magnetic Fields ◽  
Solar Magnetic Field ◽  
Charged Particles ◽  
Coronal Heating ◽  
Magnetic Control ◽  
Solar Magnetic Fields ◽  
Historical Account ◽  
Turbulent Field ◽  
Sunspot Equilibrium ◽  
General Field

A historical account of the subject's development is attempted. Prior to 1940, the most significant papers were those by Larmor (1919) and Cowling (1934) on dynamo theories of solar fields: by Kiepenheuer (1935) on the corona; and by Ferraro (1937) on isorotation. These indicated the importance of electromagnetic forces and were groping towards the idea of frozen-in fields. The latter idea was, however, not clearly stated before Alfvén's 1941–2 papers.Theory since then is divided into sections concerned with mechanical effects of magnetic fields, theories of sunspots, and the nature and origin of solar magnetic fields. The first includes theories of magnetic control of support of coronal filaments and prominences (van de Hulst, Alfvén, Dungey) and theories of magnetic influence on sunspot equilibrium. The second includes Alfvén's and Walén's theories of the solar cycle, and Biermann's explanation of sunspot coolness in terms of magnetic inhibition of convection. Sunspot theories, being discussed more fully by Biermann, are considered only briefly.Electromagnetic heating covers theories of coronal heating and flares, discharge phenomena, particle acceleration and radio emission. Many of the older theories (Alfvén's on coronal heating, Giovanelli's on flares, that of Bagge and Biermann on cosmic rays) are set aside because of their neglect of self-induction effects and inadequacy of the mechanism of conversion. The relative motion of charged particles and neutral atoms (Piddington, Cowling) is described as supplying a powerful heating effect.As regards the magnitude of the general solar magnetic field, it is suggested that the observed value can be discarded only if decisive reasons are given. Other theories having so far proved inadequate, dynamo theories of the origin of solar fields are regarded as the most promising. These can be partial, as when a toroidal field capable of explaining spot fields is supposed to be generated from the general field (Walén and others), or when a turbulent field is supposed to be generated from a smaller regular field (Alfvén and others): or total, when a simultaneous explanation of all fields is attempted (e.g. Parker). A general appraisal is made of the different theories.

scholarly journals The motion of color-charged particles as a means of testing the non-Abelian dark matter model

2019 ◽  
Vol 28 (01) ◽  
pp. 1950017 ◽  
Author(s):  
Vladimir Dzhunushaliev ◽  
Vladimir Folomeev ◽  
Nina Protsenko
Keyword(s):  
Dark Matter ◽  
Magnetic Fields ◽  
Gauge Field ◽  
Charged Particles ◽  
Analytic Solutions ◽  
Yang Mills ◽  
Electric And Magnetic Fields ◽  
Matter Model ◽  
Dark Matter Model

A possibility is discussed to experimentally test a dark matter model supported by a classic non-Abelian SU(3) Yang–Mills gauge field. Our approach is based on the analysis of the motion of color-charged particles in the background of color electric and magnetic fields using the Wong equations. Estimating the magnitudes of the color fields near the edge of a galaxy, we employ them in obtaining the general analytic solutions to the Wong equations. Using the latter, we calculate the magnitude of the extra acceleration of color-charged particles related to the possible presence of the color fields in the neighborhood of Earth.

Sign in / Sign up

Export Citation Format

Share Document