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首页> 外文期刊>Journal of Geophysical Research, A. Space Physics: JGR >Magnetosheath for almost-aligned solar wind magnetic field and flow vectors: Wind observations across the dawnside magnetosheath at X = —12 Re
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Magnetosheath for almost-aligned solar wind magnetic field and flow vectors: Wind observations across the dawnside magnetosheath at X = —12 Re

机译：磁鞘almost-aligned太阳风磁场和流矢量:风观察整个dawnside磁鞘X = -12再保险

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摘要

While there are many approximations describing the flow of the solar wind past the magnetosphere in the magnetosheath, the case of perfectly aligned (parallel or anti-parallel)interplanetary magnetic field (IMF) and solar wind flow vectors can be treated exactly in a magnetohydrodynamic (MHD) approach. In this work we examine a case of nearly-opposed (to within 15°) interplanetary field and flow vectors, which occurred on October 24-25, 2001 during passage of the last interplanetary coronal mass ejection in an ejecta merger. Interplanetary data are from the ACE spacecraft. Simultaneously Wind was crossing the near-Earth (X～ -13 Re) geomagnetic tail and subsequently made an approximately 5-hour-long magnetosheath crossing close to the ecliptic plane (Z = -0.7 Re).Geomagnetic activity was returning steadily to quiet, “ground” conditions. We first compare the predictions of the Spreiter and Rizzi theory with the. Wind magnetosheath observations and find fair agreement, in particular as regards the proportionality of the magnetic field strength and the product of the plasma density and bulk speed. We then carry out a smallperturbation analysis of the Spreiter and Rizzi solution to account for the small IMF components perpendicular to the flow vector. The resulting expression is compared to the time series of the observations and satisfactory agreement is obtained. We also present and discuss observations in the dawnside boundary layer of pulsed, high-speed (v ～ 600 km/s) flows exceeding the solar wind flow speeds. We examine various generating mechanisms and suggest that the most likely cause is a wave of frequency 3.2 ml lz excited at the inner edge of the boundary layer by the Kelvin-Helmholtz instability.
机译：虽然有很多近似描述磁气圈的太阳风流过去磁鞘,完全一致的情况下(平行或反平行)行星际磁场(IMF)和太阳风流动向量在磁流体动力完全可以治疗(磁流体动力)的方法。在15°nearly-opposed()行星际场和流矢量,这发生在10月24 - 25日,在2001年的最后一个星际日冕物质抛射喷出物合并。宇宙飞船。近地(X ~ -13 Re)和地磁的尾巴随后大约5-hour-long磁鞘穿越接近黄道飞机(Z = -0.7)。稳步恢复平静,“地面”的条件。我们首先比较Spreiter的预测组织者和Rizzi理论的。观察和发现公平协议,至于的比例磁场强度的产品等离子体密度和体积速度。Spreiter和smallperturbation分析Rizzi占小国际货币基金组织(IMF)解决方案组件垂直于流矢量。生成的表达式进行比较一系列的观察和满意协议。讨论观察dawnside边界层脉冲、高速(v ~ 600 km / s)流动超过了太阳风流动速度。各种各样的生成机制和建议最可能的原因是一波又一波的频率3.2毫升lz兴奋内部边缘的边界由Kelvin-Helmholtz层不稳定。

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