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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >Magnetosheath and heliosheath mirror mode structures, interplanetary magnetic decreases, and linear magnetic decreases: Differences and distinguishing features
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Magnetosheath and heliosheath mirror mode structures, interplanetary magnetic decreases, and linear magnetic decreases: Differences and distinguishing features

机译:磁石场和日鞘镜模式结构,行星际磁场减小,线性磁场减小:区别和区别

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摘要

There has been considerable confusion in the literature about what mirror mode (MM), magnetic decrease (MD), and linear magnetic decrease (LMD) structures are and are not. We will reexamine past spacecraft observations to demonstrate the observational similarities and differences between these magnetic and plasma structures. MM structures in planetary magnetosheaths, cometary sheaths, and the heliosheath have the following characteristics: (1) the structures have little or no changes in the magnetic field direction across the magnetic dips; (2) the structures have quasiperiodic spacings, varying from ~20 proton gyroradii (r_p) in the Earth's magnetosheath to ~57 r_p in the heliosheath; and (3) the magnetic dips have smooth edges. Magnetosheath MM structures are generated by the mirror instability where β_⊥/β_∥ > 1 + 1/β_⊥ (β is the plasma thermal pressure divided by the magnetic pressure). In general, the sources of free energy for the mirror instability are reasonably well understood: shock compression, field line draping, and, in the cases of comets and the heliosheath, also ion pickup. The observational properties of interplanetary MDs are as follows: (1) there is a broad range of magnetic field angular changes across them; (2) their thicknesses can range from as little as 2-3 r_p to thousands of r_p, with no "characteristic" size; and (3) they typically are bounded by discontinuities. The mechanism(s) for interplanetary MD generation is (are) currently unresolved, although at least five different mechanisms have been proposed in the literature. Tsurutani et al. (2009a) have argued against mirror instability for those MDs generated within interplanetary corotating interaction regions. Interplanetary LMDs are by definition a subset of MDs with small angular changes across them (θ < 10°). Are LMDs generated by the mirror instability or by another mechanism? Is it possible that there are several different types of LMDs involving different generation mechanisms? At the present time, no one knows the answers to these latter questions.
机译:关于什么是镜像模式(MM),磁减少(MD)和线性磁减少(LMD)结构,文献有相当多的困惑。我们将重新检查过去的航天器观测结果,以证明这些磁性和等离子体结构之间的观测相似性和差异。行星磁石,彗鞘和日鞘中的MM结构具有以下特征:(1)在整个磁倾角中,磁场方向的变化很小或没有变化; (2)这些结构具有准周期性的间距,范围从地球磁石的〜20质子回旋半径(r_p)到日鞘的〜57 r_p不等; (3)磁倾角边缘光滑。磁镜MM结构是由镜面不稳定性产生的,其中β_⊥/β_∥> 1 + 1 /β_⊥(β是等离子体热压除以磁压)。通常,对于镜面不稳定性的自由能来源已被很好地理解:冲击压缩,场线悬垂,并且在彗星和日鞘的情况下,还可以进行离子拾取。行星际MD的观测特性如下:(1)它们之间的磁场角变化范围很广; (2)它们的厚度范围从2-3 r_p到数千r_p,没有“特征”尺寸; (3)它们通常受到不连续性的限制。尽管文献中至少提出了五种不同的机制,但行星际MD生成的机制目前仍未解决。鹤谷等。 (2009a)反对在行星际同旋转相互作用区域内产生的那些MD的镜像不稳定性。根据定义,行星际LMD是MD的子集,它们之间的角度变化很小(θ<10°)。 LMD是由镜像不稳定还是由其他机制生成的?是否有几种不同类型的LMD涉及不同的生成机制?目前,还没有人知道这些后一个问题的答案。

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