scholarly journals On the stability of thoriated tungsten cathodes in strong magnetic fields

2021 ◽  
Vol 92 (8) ◽  
pp. 083510
Author(s):  
U. Wenzel ◽  
G. Schlisio ◽  
T. S. Pedersen ◽  
M. Marquardt ◽  
D. Pilopp ◽  
...  
Keyword(s):  
Magnetic Fields ◽  
Strong Magnetic Fields ◽  
Thoriated Tungsten ◽  
The Stability

Strong magnetic fields

1960 ◽  
Vol 70 (4) ◽  
pp. 693-714 ◽  
Author(s):  
G.M. Strakhovskii ◽  
N.V. Kravtsov
Keyword(s):  
Magnetic Fields ◽  
Strong Magnetic Fields

Magnetic molecular nanoclusters in strong magnetic fields

2002 ◽  
Vol 172 (11) ◽  
pp. 1303 ◽  
Author(s):  
Anatolii K. Zvezdin ◽  
Viktor V. Kostyuchenko ◽  
V.V. Platonov ◽  
V.I. Plis ◽  
A.I. Popov ◽  
...  
Keyword(s):  
Magnetic Fields ◽  
Strong Magnetic Fields

scholarly journals The measurement of the energy of cosmic rays - II—The curvature measurements and the energy spectrum

1936 ◽  
Vol 154 (883) ◽  
pp. 573-587 ◽  
Keyword(s):  
Magnetic Field ◽  
Energy Spectrum ◽  
Cosmic Rays ◽  
Magnetic Fields ◽  
Strong Magnetic Fields ◽  
The Earth ◽  
Primary Particles ◽  
Curvature Measurements

Both the penetrating power of the cosmic rays through material ab­sorbers and their ability to reach the earth in spite of its magnetic field, make it certain that the energy of many of the primary particles must reach at least 10 11 e-volts. However, the energy measurements by Kunze, and by Anderson, using cloud chambers in strong magnetic fields, have extended only to about 5 x 10 9 e-volts. Particles of greater energy were reported, but the curvature of their tracks was too small to be measured with certainty. We have extended these energy measurements to somewhat higher energies, using a large electro-magnet specially built for the purpose and described in Part I. As used in these experiments, the magnet allowed the photography of tracks 17 cm long in a field of about 14,000 gauss. The magnet weighed about 11,000 kilos and used a power of 25 kilowatts.

scholarly journals No-z Model for Magnetic Fields of Different Astrophysical Objects and Stability of the Solutions

Data ◽  
2021 ◽  
Vol 6 (1) ◽  
pp. 4
Author(s):  
Evgeny Mikhailov ◽  
Daniela Boneva ◽  
Maria Pashentseva
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Large Scale ◽  
Point Of View ◽  
Accretion Discs ◽  
Wide Range ◽  
Astrophysical Objects ◽  
Alpha Effect ◽  
The Stability ◽  
The Magnetic Field

A wide range of astrophysical objects, such as the Sun, galaxies, stars, planets, accretion discs etc., have large-scale magnetic fields. Their generation is often based on the dynamo mechanism, which is connected with joint action of the alpha-effect and differential rotation. They compete with the turbulent diffusion. If the dynamo is intensive enough, the magnetic field grows, else it decays. The magnetic field evolution is described by Steenbeck—Krause—Raedler equations, which are quite difficult to be solved. So, for different objects, specific two-dimensional models are used. As for thin discs (this shape corresponds to galaxies and accretion discs), usually, no-z approximation is used. Some of the partial derivatives are changed by the algebraic expressions, and the solenoidality condition is taken into account as well. The field generation is restricted by the equipartition value and saturates if the field becomes comparable with it. From the point of view of mathematical physics, they can be characterized as stable points of the equations. The field can come to these values monotonously or have oscillations. It depends on the type of the stability of these points, whether it is a node or focus. Here, we study the stability of such points and give examples for astrophysical applications.

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