Transport Phenomena in a Completely Ionized Gas in Presence of a Magnetic Field

Landshoff, Rolf

doi:10.1103/physrev.76.904

Cited by 170 publications

(38 citation statements)

References 1 publication

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“…1. In the collisional limit (k → 0), the coefficients reproduce the classical transport coefficients [1,2,11]:σ → 1.98 ≃σ LS ,α → −1.39, andκ → 4.18 which agree with the convergent values from the moment approach [12].…”

Section: Electron Parallel Transportsupporting

confidence: 62%

“…For a sinusoidal drive of wavelength λ, L = λ/2π and k = 2πλ C /λ. For high-collisionality (k ≪ 1) plasmas, the electron parallel transport is described by the Spitzer theory [1,2], where the flux densities are connected to thermodynamic drives by transport coefficients. For intermediate to low collisionality, integral (nonlocal) transport effects are considered in Refs.…”

Section: Introductionmentioning

confidence: 99%

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Electron parallel transport for arbitrary collisionality

Yun

et al. 2017

Physics of Plasmas

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the electric current and heat flux densities are connected to the modified electric field and temperature gradient by transport coefficients. In contrast to the classical theory, the dimensionless coefficients depend on the collisionality quantified by a Knudsen number, the ratio of the collision length to the angular wavelength.The key difference comes from the proper treatment of the viscosity and friction terms in the momentum balance equation, accurately reflecting the free streaming and collision terms in the kinetic equation. For an arbitrary fluctuation, the transport relations may be expressed by a Fourier series or transform. For low collisionality, the electric resistivity can be significantly larger than that of classical theory and may predict the correct timescale for fast magnetic reconnection.

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Section: Electron Parallel Transportsupporting

confidence: 62%

Section: Introductionmentioning

confidence: 99%

Electron parallel transport for arbitrary collisionality

Yun

et al. 2017

Physics of Plasmas

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“…Although it was recognized as early as 1949 that a magnetic field could significantly reduce electron thermal conductivity, 3 it was several years after the seminal paper 4 proposing ICF that magnetized fuel was proposed 5 and the first experiments demonstrating that a magnetic field could improve ICF yields were performed. 6 An intense relativistic electron beam was used to drive capsule implosions in these experiments.…”

Section: Introductionmentioning

confidence: 99%

Pulsed-power-driven cylindrical liner implosions of laser preheated fuel magnetized with an axial field

Slutz¹,

Herrmann²,

Vesey³

et al. 2010

Physics of Plasmas

541

328

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The radial convergence required to reach fusion conditions is considerably higher for cylindrical than for spherical implosions since the volume is proportional to r2 versus r3, respectively. Fuel magnetization and preheat significantly lowers the required radial convergence enabling cylindrical implosions to become an attractive path toward generating fusion conditions. Numerical simulations are presented indicating that significant fusion yields may be obtained by pulsed-power-driven implosions of cylindrical metal liners onto magnetized (>10 T) and preheated (100–500 eV) deuterium-tritium (DT) fuel. Yields exceeding 100 kJ could be possible on Z at 25 MA, while yields exceeding 50 MJ could be possible with a more advanced pulsed power machine delivering 60 MA. These implosions occur on a much shorter time scale than previously proposed implosions, about 100 ns as compared to about 10 μs for magnetic target fusion (MTF) [I. R. Lindemuth and R. C. Kirkpatrick, Nucl. Fusion 23, 263 (1983)]. Consequently the optimal initial fuel density (1–5 mg/cc) is considerably higher than for MTF (∼1 μg/cc). Thus the final fuel density is high enough to axially trap most of the α-particles for cylinders of approximately 1 cm in length with a purely axial magnetic field, i.e., no closed field configuration is required for ignition. According to the simulations, an initial axial magnetic field is partially frozen into the highly conducting preheated fuel and is compressed to more than 100 MG. This final field is strong enough to inhibit both electron thermal conduction and the escape of α-particles in the radial direction. Analytical and numerical calculations indicate that the DT can be heated to 200–500 eV with 5–10 kJ of green laser light, which could be provided by the Z-Beamlet laser. The magneto-Rayleigh-Taylor (MRT) instability poses the greatest threat to this approach to fusion. Two-dimensional Lasnex simulations indicate that the liner walls must have a substantial initial thickness (10–20% of the radius) so that they maintain integrity throughout the implosion. The Z and Z-Beamlet experiments are now being planned to test the various components of this concept, e.g., the laser heating of the fuel and the robustness of liner implosions to the MRT instability.

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“…For this purposes, however, we need of detailed function of temperature and magnetic field dependence of plasma kinetic coefficients. Such investigations started seventy years ago by R. Landshoff [47], E. S. Fradkin in 1951 [48], I. E. Tamm [49] and S. I. Braginskii in 1952 [50]. The main final results are listed in the Kinetics by Lifshitz and Pitaevskii [23].…”

Section: Plasma Heating By Aw -A Historical Perspectivementioning

confidence: 96%

Magnetohydrodynamic calculation of the temperature and wind velocity profile of the solar transition region. Preliminary results.

et al. 2018

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Abstract. The sharp almost step like increase the temperature in the transition region (TR) between chromosphere and solar corona is well-known from decades; for first time we are giving a detailed magnetohydrodynamic (MHD) calculation of the height dependence of the temperature. The width of the transition region is evaluated by maximal value of the logarithmic derivative of the temperature. At fixed heating, only MHD can give such a narrow width and in such sense, even the qualitative agreement with the observational data, gives the final verdict what the heating mechanism of the solar corona is. Static profiles of the temperature and wind velocity are calculated for static frequency dependent spectral density of the incoming MHD waves; no time dependent computer simulations. At fixed spectral density of MHD waves, the MHD calculation predicts height dependence of the non-thermal broadening of spectral lines and its angular dependence. For illustration is used one dimensional approximation of completely ionized hydrogen plasma in weak magnetic field, but it is considered that the width of the TR is weakly dependent with respect of further elaboration. The analyzed MHD calculation is a numerical confirmation of the qualitative concept of self-induced opacity of the plasma with respect to MHD waves. The plasma viscosity strongly increases with the temperature. Heated by MHD waves, plasma increases the wave absorption and this positive feedback leads to further heating. The static temperature profile is a result of a self-consistent calculation of propagation of MHD wave through the static background of wind and temperature profile. The numerical method allows consideration of incoming MHD waves with an arbitrary spectral density. Further elaboration of the method are briefly discussed: influence of second viscosity in the chromospheric part of the TR, influence of the magnetic field on the coronal side of the TR and investigation of such type effects on the width of the TR. Alfvén model for corona heatingThe discovery of the 5303 Å green 1 of Fe 13+ and 6374 Å red 2 of Fe 9+ magneto-dipole transition lines in the solar corona spectrum [1] posed an important problem for the fundamental physics -what is the mechanism of the heating of the solar corona and why the temperature of the corona is 100 times

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Transport Phenomena in a Completely Ionized Gas in Presence of a Magnetic Field

Cited by 170 publications

References 1 publication

Electron parallel transport for arbitrary collisionality

Electron parallel transport for arbitrary collisionality

Pulsed-power-driven cylindrical liner implosions of laser preheated fuel magnetized with an axial field

Magnetohydrodynamic calculation of the temperature and wind velocity profile of the solar transition region. Preliminary results.

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