Effect of a magnetic field on the radiation emitted by a nonequilibrium hydrogen and deuterium plasma

2001 ◽  
Vol 92 (3) ◽  
pp. 441-453 ◽  
Author(s):  
V. G. Novikov ◽  
V. S. Vorob’ev ◽  
L. G. D’yachkov ◽  
A. F. Nikiforov
Keyword(s):  
Magnetic Field ◽  
Deuterium Plasma

Development of a 56 GHz ECH system for deuterium plasma experiments of a low magnetic field in LHD

2021 ◽  
Vol 173 ◽  
pp. 112862
Author(s):  
R. Yanai ◽  
T. Ii Tsujimura ◽  
S. Kubo ◽  
Y. Yoshimura ◽  
T. Takeuchi ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Deuterium Plasma ◽  
Low Magnetic Field

On the Acceleration of the Particle Flux of Laser Deuterium Plasma in a Fast-Growing Magnetic Field

2018 ◽  
Vol 15 (7) ◽  
pp. 990-993 ◽  
Author(s):  
K. I. Kozlowski ◽  
A. E. Shikanov ◽  
E. D. Vovchenko ◽  
A. A. Isaev
Keyword(s):  
Magnetic Field ◽  
Particle Flux ◽  
Deuterium Plasma ◽  
Fast Growing

Heating of a Theta-Pinch Plasma by a CO2 Laser

1971 ◽  
Vol 49 (12) ◽  
pp. 1685-1687 ◽  
Author(s):  
J. Martineau ◽  
H. Pépin
Keyword(s):  
Magnetic Field ◽  
Laser Pulse ◽  
Pulse Duration ◽  
Co2 Laser ◽  
Magnetic Confinement ◽  
Deuterium Plasma ◽  
Ion Temperature ◽  
Theta Pinch ◽  
Absorbed Power ◽  
The Magnetic Field

The heating of a theta-pinch deuterium plasma by a CO2 laser has been studied as a function of pulse duration and energy. A hydrodynamical approach was used with temperatures and densities assumed uniform in a fully ionized plasma. This model takes into account the dynamics of the magnetic field, the axial and radial magnetic confinement, the shape of the laser pulse, and energy transferred to the plasma by inverse bremsstrahlung. We discuss the results (dimensions, temperature, absorbed power) snowing that an increase in pulse duration results in higher electron and ion temperature.

Magnetic-field strengths from optical polarization data

1967 ◽  
Vol 31 ◽  
pp. 381-383
Author(s):  
J. M. Greenberg
Keyword(s):  
Magnetic Field ◽  
Optical Polarization ◽  
Polarization Data ◽  
Term Model ◽  
Source Of Information ◽  
Field Strengths

Van de Hulst (Paper 64, Table 1) has marked optical polarization as a questionable or marginal source of information concerning magnetic field strengths. Rather than arguing about this–I should rate this method asq+-, or quarrelling about the term ‘model-sensitive results’, I wish to stress the historical point that as recently as two years ago there were still some who questioned that optical polarization was definitely due to magnetically-oriented interstellar particles.

Observing the galactic magnetic field

1967 ◽  
Vol 31 ◽  
pp. 375-380
Author(s):  
H. C. van de Hulst
Keyword(s):  
Magnetic Field ◽  
Fair Agreement ◽  
Solar Neighbourhood ◽  
Galactic Magnetic Field ◽  
The Magnetic Field

Various methods of observing the galactic magnetic field are reviewed, and their results summarized. There is fair agreement about the direction of the magnetic field in the solar neighbourhood:l= 50° to 80°; the strength of the field in the disk is of the order of 10-5gauss.

Structure in the radiation of the galactic disk

1967 ◽  
Vol 31 ◽  
pp. 355-356
Author(s):  
R. D. Davies
Keyword(s):  
Magnetic Field ◽  
Galactic Disk ◽  
Galactic Magnetic Field ◽  
Measured Polarization

Observations at various frequencies between 136 and 1400 MHz indicate a considerable amount of structure in the galactic disk. This result appears consistent both with measured polarization percentages and with considerations of the strength of the galactic magnetic field.

Calculated Coronal Magnetic Fields and Their Comparison with the Coronal Structures as Observed during Five Solar Eclipses

1994 ◽  
Vol 144 ◽  
pp. 559-564
Author(s):  
P. Ambrož ◽  
J. Sýkora
Keyword(s):  
Magnetic Field ◽  
Solar Cycle ◽  
Magnetic Fields ◽  
Solar Corona ◽  
Coronal Magnetic Field ◽  
Coronal Magnetic Fields ◽  
Solar Eclipses ◽  
Coronal Structures

AbstractWe were successful in observing the solar corona during five solar eclipses (1973-1991). For the eclipse days the coronal magnetic field was calculated by extrapolation from the photosphere. Comparison of the observed and calculated coronal structures is carried out and some peculiarities of this comparison, related to the different phases of the solar cycle, are presented.

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