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首页> 外文期刊>Plasma physics and controlled fusion >Modelling energetic particles by a relativistic kappa-loss-cone distribution function in plasmas
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Modelling energetic particles by a relativistic kappa-loss-cone distribution function in plasmas

机译：通过相对论的等离子κ损失锥分布函数模拟高能粒子

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摘要

Energetic particles found in planetary magnetospheres and other plasmas, where mirror geometries occur, often exhibit two typical characteristics: a pronounced high energy tail and an anisotropy. A relativistic kappa-loss-cone (KLC) distribution function f(kappa L) is initially developed which incorporates features of the well-known kappa type and loss-cone type, i.e. the anisotropy behaves as a loss-cone distribution; the energy satisfies proportional to [1u(2)]((kappa,1)) for a relatively large velocity nu as a kappa distribution f(kappa) does and spreads proportional to [1/p](kappa+1) at the relativistic energies (where kappa and p are the energy spectral index and the particle momentum, respectively). This indicates that the new distribution f(kappa L) obeys the power-law not only at the lower energies but also at the relativistic energies since the relativistic energy proportional to p. Numerical calculations are performed for a direct comparison between the new KLC distribution and the current kappa distribution, respectively. It is found that the regular kappa distribution generally decreases faster than the KLC distribution with the kinetic energy E-k especially when theta(2) increases (where theta(2) is the energy weight parameter), e-g. f(kappa)/f(kappa L) <= 10(-2) for E-k >= 2.0 MeV and theta(2) >= 0.25. However, no big difference occurs between both distributions through energies up to similar to 500 keV for theta(2) <= 0.025. Furthermore, the regular kappa distribution containing either the temperature anisotropy or both the loss cone and temperature anisotropy is quite different from the KLC distribution. The new KLC distribution may be applicable to the outer radiation belts of the Earth, the inner Jovian magnetosphere and other plasmas (including the laboratory machine) where relativistic particles are present.
机译：在存在镜像几何形状的行星磁层和其他等离子体中发现的高能粒子通常表现出两个典型特征：明显的高能尾和各向异性。最初开发了相对论的kappa损耗圆锥（KLC）分布函数f（kappa L），该函数结合了众所周知的kappa型和损耗圆锥型的特征，即各向异性表现为损耗圆锥分布。对于相对较大的速度nu，能量满足[1 / nu（2）]（（kappa，1））的比例，而kappa分布f（kappa）的能量却与[1 / p]（kappa + 1）的比例成正比相对论能量（其中κ和p分别是能谱指数和质点动量）。这表明新的分布f（kappa L）不仅在低能量处服从幂律，而且在相对论能量处服从幂律，因为相对论能量与p成正比。分别进行数值计算以直接比较新的KLC分布和当前的kappa分布。发现规则的κ分布通常比具有动能E-k的KLC分布更快，特别是当θ（2）增加（其中θ（2）是能量权重参数）e-g时。对于E-k> = 2.0 MeV和theta（2）> = 0.25，f（kappa）/ f（k L）L == 10（-2）。但是，对于theta（2）<= 0.025，通过高达500 keV的能量，两种分布之间都没有大的差异。此外，包含温度各向异性或损耗锥和温度各向异性的规则kappa分布与KLC分布完全不同。新的KLC分布可能适用于存在相对论粒子的地球外部辐射带，内部木星磁层和其他等离子体（包括实验室机器）。

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