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Spectral characteristics of the collisional stationary Alfven wave in the laboratory and space regimes

机译：碰撞阿尔夫文固定波在实验室和空间范围内的光谱特性

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摘要

Solutions of the collisional stationary Alfven (StA) wave equations are presented for both laboratory and space plasma parameter regimes. The stationary inertial Alfven (StIA) wave is a time-independent electromagnetic structure generated by plasma convection (V-d = E/B-0) across field-aligned current sheets in a cold (T-e = T-i = 0) background plasma (Knudsen 1996 J. Geophys. Res. 101 10761). The StIA wave can accelerate electrons in the magnetic field-aligned direction to speeds in excess of the local Alfven speed. Recently, the model of the StIA wave was generalized to include the effects of electron and ion collisional resistivity, as well as non-zero thermal pressure (Finnegan et al 2008 Phys. Plasmas at press). Here, the laboratory-relevant regime is evaluated. Solutions to the StA wave equations are presented for plasma parameters typical of the main-discharge and after-glow plasmas of the LArge Plasma Device at UCLA's Basic Plasma Science Facility. Cases for which the background plasma density is either enhanced or depleted by the StA wave are distinguished. Coulomb collisions are predicted to be important in damping the StA wave in the after-glow plasma and in supporting solitary density enhancements in the main-discharge plasma. The space regime is also evaluated. We present solutions to the StA wave equations for typical plasma parameters associated with the topside ionosphere and the solar corona. For typical plasma parameters in the topside ionosphere (Alt.similar to 1500 km), StA wave solutions are characterized by the parallel component of electric field E-parallel to and plasma density, the spatial modulation of which are in good agreement with measurements associated with Alfvenic structures made previously by the Freja satellite. For plasma parameters typical of the solar corona, it is shown that the StA wave may provide a physical mechanism for generating small scale (similar to 10m across), adjacent, magnetic-field-aligned, current channels of alternating polarity in the solar corona.
机译：针对实验室和空间等离子体参数方案，提出了固定式碰撞Alfven（StA）波动方程的解。静止惯性Alfven（StIA）波是由时间对流的电磁结构（Vd = E / B-0）在冷（Te = Ti = 0）背景等离子体（Knudsen 1996 J （Geophys.Res.101 10761）。 StIA波可以使电子在磁场对准的方向上加速，其速度超过局部Alfven速度。最近，StIA波的模型得到了概括，包括电子和离子碰撞电阻率以及非零热压的影响（Finnegan等，2008年出版的《物理等离子》）。在这里，评估与实验室有关的制度。针对加州大学洛杉矶分校的基本等离子科学设施中LArge等离子设备的主要放电和余辉等离子体的典型等离子体参数，提出了StA波动方程的解。区分背景血浆密度被StA波增强或耗尽的情况。预计库仑碰撞对于衰减辉光后等离子体中的StA波和支持主放电等离子体中的孤立密度增强非常重要。还评估了空间状况。我们提出了与顶部电离层和太阳电晕相关的典型等离子体参数的StA波方程的解决方案。对于顶面电离层中的典型等离子体参数（Alt。类似于1500 km），StA波解的特征是电场平行于电场分量E平行于等离子体密度，其空间调制与与以前由Freja卫星制造的高空结构。对于典型的太阳电晕等离子体参数，表明StA波可能提供了一种物理机制，用于在太阳电晕中生成小尺度（跨度约10m），相邻，磁场对齐，极性交替的电流通道。

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