scholarly journals GV/cm scale laser-magnetic resonant acceleration in vacuum

2017 ◽  
Vol 35 (3) ◽  
pp. 520-527 ◽  
Author(s):  
Y. Zhang ◽  
J.-L. Jiao ◽  
B. Zhang ◽  
Z.-M. Zhang ◽  
Y.-Q. Gu
Keyword(s):  
Magnetic Field ◽  
Phase Difference ◽  
Electron Bunch ◽  
Longitudinal Magnetic Field ◽  
Laser Intensity ◽  
Resonant Condition ◽  
Electron Accelerators ◽  
Simulation Results ◽  
Spatial Size ◽  
Resonant Acceleration

AbstractResonant acceleration of electrons by a laser in the background of an extra longitudinal magnetic field is investigated analytically and numerically. The resonant condition is independent of laser intensity, and when satisfied, the energy gain is proportional to $a_0^2 $ and the square of phase difference. This process is mainly limited by the magnitude and spatial size of the extra magnetic field. Under the laboratory conditions, simulation results show that a monoenergetic and collimated electron bunch can still be obtained in ~ GV/cm scale, which sheds a light on the vacuum table-top laser-driven electron accelerators.

THE EXPERIMENTALLY OBSERVED OPTICAL COTTON–MOUTON EFFECT: EVIDENCE FOR THE PHOTON'S LONGITUDINAL MAGNETIC FIELD, B(3)

1993 ◽  
Vol 07 (19) ◽  
pp. 1247-1251 ◽  
Author(s):  
M. W. EVANS
Keyword(s):  
Magnetic Field ◽  
Laser Beam ◽  
Flux Density ◽  
Experimental Observation ◽  
Longitudinal Magnetic Field ◽  
Laser Intensity ◽  
Longitudinal Component ◽  
Second Order ◽  
Permanent Magnetic Field ◽  
Classical Counterpart

The recent experimental observation of the optical Cotton–Mouton effect is consistent with the induction of magnetization by the longitudinal component of the photon's magnetic field, whose classical counterpart is the equivalent flux density B(3). In the optical Cotton–Mouton effect observed by Zon et al.,16 the field B(3) acts at second order and is independent of the polarization of the inducing laser beam propagating parallel to a permanent magnetic field. The optical Cotton–Mouton effect is therefore proportional to the laser intensity as observed.16

scholarly journals Resonant acceleration of electrons by intense circularly polarized Gaussian laser pulses

2008 ◽  
Vol 26 (1) ◽  
pp. 51-60 ◽  
Author(s):  
H.Y. Niu ◽  
X.T. He ◽  
B. Qiao ◽  
C.T. Zhou
Keyword(s):  
Plasma Density ◽  
Relativistic Electron Beam ◽  
Laser Intensity ◽  
Laser Pulses ◽  
High Energy ◽  
Relative Energy ◽  
Resonant Condition ◽  
Circularly Polarized ◽  
Laser Group ◽  
Resonant Acceleration

AbstractResonant acceleration of plasma electrons in combined circularly polarized Gaussian laser fields and self-generated quasistatic fields has been investigated theoretically and numerically. The latter includes the radial quasistatic electric field, the azimuthal quasistatic magnetic field and the axial one. The resonant condition is theoretically given and numerically testified. The results show some of the resonant electrons are accelerated to velocities larger than the laser group velocity and thus gain high energy. For peak laser intensity I0 = 1 × 1020 W cm−2 and plasma density n0 = 0.1ncr, the relativistic electron beam with energies increased from 207 MeV to 262 MeV with a relative energy width around 24% and extreme low beam divergence less than 1° has been obtained. The effect of laser intensity and plasma density on the final energy gain of resonant electrons is also investigated.

Design and Simulation of Solenoid for Buncher of a Linear Accelerator

2010 ◽  
Author(s):  
Ehsan Ebrahimi Basabi ◽  
Feryidoon Abbasi Davani
Keyword(s):  
Magnetic Field ◽  
Linear Accelerator ◽  
Longitudinal Magnetic Field ◽  
Cooling System ◽  
Heat Power ◽  
Light Velocity ◽  
Considerable Fraction ◽  
Applied Forces ◽  
Simulation Results ◽  
Set Up

One of the most important components of a linac is buncher. Throughout most of the buncher, the electrons are well forward of the crest and have velocities considerably less than light velocity, thus they are in a region of radial defocusing and a considerable fraction of the beam will be lost unless defocusing action is counteracted by some other applied forces. The simplest way to do this is to set up a longitudinal magnetic field which interacts with the radial motion of the electrons and causes them to follow helical orbits through the space occupied by the field. In this paper, five solenoids were designed to provide necessary magnetic field inside the buncher. Magnetic field was analytically calculated and compared with simulation results of CST. Because of resistance in wires, some amount of energy appears in form of heat, so heat power was calculated analytically and cooling system was designed for these solenoids by ANSYS.

Refinement of metal structure in arc surfacing under the effect of longitudinal magnetic field

2019 ◽  
Vol 2019 (2) ◽  
pp. 19-21
Author(s):  
A.D. Razmyshlyaev ◽  
◽  
M.V. Ageeva ◽  
E.V. Lavrova ◽  
◽  
...  
Keyword(s):  
Magnetic Field ◽  
Longitudinal Magnetic Field ◽  
Metal Structure

scholarly journals Design and evaluation of 10-kA class superconducting DC power cable based on longitudinal magnetic field effect

2021 ◽  
Vol 1975 (1) ◽  
pp. 012037
Author(s):  
Y Kinoshita ◽  
T Yonenaka ◽  
Y Ichiki ◽  
T Akasaka ◽  
E S Otabe ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Field Effect ◽  
Longitudinal Magnetic Field ◽  
Magnetic Field Effect ◽  
Power Cable ◽  
Dc Power

scholarly journals Simulations of Switchback, Fragmentation and Sunspot Pair in δ-Sunspots during Magnetic Flux Emergence

Sensors ◽  
2021 ◽  
Vol 21 (2) ◽  
pp. 586
Author(s):  
Che-Jui Chang ◽  
Jean-Fu Kiang
Keyword(s):  
Magnetic Field ◽  
Solar System ◽  
Field Strength ◽  
Magnetic Flux ◽  
Initial Conditions ◽  
Observation Data ◽  
Flux Emergence ◽  
Polarity Inversion ◽  
Simulation Results ◽  
Spot Type

Strong flares and coronal mass ejections (CMEs), launched from δ-sunspots, are the most catastrophic energy-releasing events in the solar system. The formations of δ-sunspots and relevant polarity inversion lines (PILs) are crucial for the understanding of flare eruptions and CMEs. In this work, the kink-stable, spot-spot-type δ-sunspots induced by flux emergence are simulated, under different subphotospheric initial conditions of magnetic field strength, radius, twist, and depth. The time evolution of various plasma variables of the δ-sunspots are simulated and compared with the observation data, including magnetic bipolar structures, relevant PILs, and temperature. The simulation results show that magnetic polarities display switchbacks at a certain stage and then split into numerous fragments. The simulated fragmentation phenomenon in some δ-sunspots may provide leads for future observations in the field.

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