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首页> 外文期刊>The Open Plasma Physics Journal >Interplanetary Plasma Scattering Diagnostics from Anisotropy-timeProfiles of Solar Energetic Particles
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Interplanetary Plasma Scattering Diagnostics from Anisotropy-timeProfiles of Solar Energetic Particles

机译：从太阳高能粒子的各向异性时间剖面进行行星际等离子体散射诊断

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摘要

The anisotropy-time profile of solar particle events provides a powerful diagnostics tool to the interplanetary plasma scattering parameters of energetic charged particles. In the weak focusing limit of the transport of solar particles in axisymmetric MHD turbulence, the particle anisotropy consists of two contributions, the streaming and the Compton-Getting contribution, resulting from the parallel spatial gradient and the momentum gradient of the isotropic part of the particles’ phase space density, respectively. These gradients can be calculated from the appropriate solution to the timedependent focused transport equation of solar particles. For the illustrative case of the solution of the one-dimensional time-dependent focused transport equation with a constant focusing length and a point-like instantaneous injection of particles the streaming and Compton-Getting contributions to the anisotropy-time profile are analytically calculated in MHD turbulence consisting of isospectral undamped slab Alfven waves for equal magnetic helicity. The Compton-Getting contribution scales proportional to the ratio of interplanetary Alfven speed to solar particle speed, and therefore is much smaller than the streaming contribution for the observed mildly relativistic solar particles. After vanishing anisotropy values at times t < tM the streaming anisotropy suddenly attains its maximum value AS,max = at tM = t0 + (z–z0)/v. At later times the streaming anisotropy decreases oc(t–t0)-1 approaching the asymptotic finite value (λ(p)/2L) for t–t0→∞, positive or negative, depending on the sign of the focusing length L. The new analytical form of the streaming anisotropy provides an excellent fit to the observed anisotropy profiles from the easter solar particle event of 2001 April 15 for 1.3 GeV protons, but does not well reproduce the anisotropies of 510 keV electrons.
机译：太阳粒子事件的各向异性时间剖面为高能带电粒子的行星际等离子体散射参数提供了强大的诊断工具。在轴对称MHD湍流中太阳粒子输运的弱聚焦极限下，粒子的各向异性由粒子的各向同性部分的平行空间梯度和动量梯度产生，由流和Compton-Getting贡献两个部分组成。相空间密度分别。可以从适当的解到与时间相关的太阳能粒子聚焦传输方程来计算这些梯度。对于具有恒定聚焦长度和点状瞬时注入粒子的一维时间相关聚焦输运方程的解的说明性情况，在MHD中解析计算了各向异性时间分布的流和Compton-Getting贡献。湍流由等谱的无阻尼平板Alfven波组成，具有相同的磁螺旋度。 Compton-Getting贡献比例与行星际Alfven速度与太阳粒子速度之比成正比，因此，它远小于观测到的相对论性太阳粒子的流动贡献。在时间t

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