MAGNETIC FIELD GENERATION IN CORE-SHEATH JETS VIA THE KINETIC KELVIN-HELMHOLTZ INSTABILITY

В динамической модели -динамо с переменной интенсивностью -генератора моделируются инверсии магнитного поля. Изменение интенсивности -генератора как следствие синхронизации высших мод поля скоростей и магнитного поля регулируется функцией Z(t) со степенным ядром. Получены режимы динамо для двух видов радиальной составляющей в скалярной параметризации -эффекта. Проведён анализ результатов в зависимости от изменения показателя степени ядра функции Z(t), а также сравнительный анализ с результатами исследования 10, где использовано показательное ядро функциии Z(t). In the dynamic model -dimensions are simulated reversions of the magnetic field with a varying intensity of the -generator. The change of the -generator intensity as a result of synchronization of higher modes of the velocity field and the magnetic field is regulated by a function Z(t) with a power kernel. Dynamo modes are obtained for two types of radial component in the scalar parameterization of the -effect. The results were analyzed depending on the change in the exponent of the kernel of the function Z(t), also a comparative analysis with the results of the study 10, where the exponential kernel of the function Z(t) was used.

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Pulsed magnetic field generation system for laser-plasma research

Review of Scientific Instruments ◽

10.1063/5.0035302 ◽

2021 ◽

Vol 92 (12) ◽

pp. 123506

Author(s):

A. G. Luchinin ◽

V. A. Malyshev ◽

E. A. Kopelovich ◽

K. F. Burdonov ◽

M. E. Gushchin ◽

...

Keyword(s):

Magnetic Field ◽

Laser Plasma ◽

Pulsed Magnetic Field ◽

Generation System ◽

Magnetic Field Generation ◽

Field Generation ◽

Plasma Research

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Magnetisation of partially ionised dusty disks

Journal of Plasma Physics ◽

10.1017/s0022377801001490 ◽

2001 ◽

Vol 66 (3) ◽

pp. 213-222 ◽

Cited By ~ 1

Author(s):

GUIDO T. BIRK ◽

A. KOPP ◽

H. LESCH

Keyword(s):

Magnetic Field ◽

Circumstellar Disks ◽

The Self ◽

Charged Dust ◽

Generation Process ◽

Magnetic Field Generation ◽

Field Generation ◽

Neutral Gas ◽

Fluid Velocities ◽

Dust Component

The self-magnetisation of circumstellar disks is considered within an appropriate multifluid description. These disks are composed of ionised and neutral gas as well as of a charged dust component. The most important equation in this context is the general Ohm’s law that includes a magnetic field generation term due to relative dust–neutral fluid velocities. We show that circumstellar disks can carry their own significant magnetic fields. As long as the stellar gravitation sustains the accretion flow, the self-magnetisation of the disk does not saturate until the field strength reaches its local equipartition value. The magnetic field generation process is illustrated by idealised multifluid simulations that are not restricted to a kinematic description, but model the process in a self-consistent way.

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Magnetic field generation in a jet-sheath plasma via the kinetic Kelvin-Helmholtz instability

Annales Geophysicae ◽

10.5194/angeo-31-1535-2013 ◽

2013 ◽

Vol 31 (9) ◽

pp. 1535-1541 ◽

Cited By ~ 14

Author(s):

K.-I. Nishikawa ◽

P. Hardee ◽

B. Zhang ◽

I. Duţan ◽

M. Medvedev ◽

...

Keyword(s):

Magnetic Field ◽

Growth Rate ◽

Magnetic Fields ◽

Electric Field ◽

Flow Direction ◽

Transverse Magnetic ◽

Velocity Shear ◽

Helmholtz Instability ◽

Magnetic Field Generation ◽

Relativistic Jet

Abstract. We have investigated the generation of magnetic fields associated with velocity shear between an unmagnetized relativistic jet and an unmagnetized sheath plasma. We have examined the strong magnetic fields generated by kinetic shear (Kelvin–Helmholtz) instabilities. Compared to the previous studies using counter-streaming performed by Alves et al. (2012), the structure of the kinetic Kelvin–Helmholtz instability (KKHI) of our jet-sheath configuration is slightly different, even for the global evolution of the strong transverse magnetic field. In our simulations the major components of growing modes are the electric field Ez, perpendicular to the flow boundary, and the magnetic field By, transverse to the flow direction. After the By component is excited, an induced electric field Ex, parallel to the flow direction, becomes significant. However, other field components remain small. We find that the structure and growth rate of KKHI with mass ratios mi/me = 1836 and mi/me = 20 are similar. In our simulations saturation in the nonlinear stage is not as clear as in counter-streaming cases. The growth rate for a mildly-relativistic jet case (γj = 1.5) is larger than for a relativistic jet case (γj = 15).

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