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首页> 外文期刊>The Astrophysical Journal. Letters >Weakened Magnetization and Onset of Large-scale Turbulence in the Young Solar Wind-Comparisons of Remote Sensing Observations with Simulation
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Weakened Magnetization and Onset of Large-scale Turbulence in the Young Solar Wind-Comparisons of Remote Sensing Observations with Simulation

机译：遥感观测中遥感观测的遥感观测中的遥感观测中大型太阳能紊乱的磁化和大规模湍流的发作弱化

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摘要

Recent analysis of Solar-Terrestrial Relations Observatory (STEREO) imaging observations have described the early stages of the development of turbulence in the young solar wind in solar minimum conditions. Here we extend this analysis to a global magnetohydrodynamic (MHD) simulation of the corona and solar wind based on inner boundary conditions, either dipole or magnetogram type, that emulate solar minimum. The simulations have been calibrated using Ulysses and 1 au observations, and allow, within a well-understood context, a precise determination of the location of the Alfvén critical surfaces and the first plasma beta equals unity surfaces. The compatibility of the the STEREO observations and the simulations is revealed by direct comparisons. Computation of the radial evolution of second-order magnetic field structure functions in the simulations indicates a shift toward more isotropic conditions at scales of a few Gm, as seen in the STEREO observations in the range 40-60 R_⊙. We affirm that the isotropization occurs in the vicinity of the first beta unity surface. The interpretation based on early stages of in situ solar wind turbulence evolution is further elaborated, emphasizing the relationship of the observed length scales to the much smaller scales that eventually become the familiar turbulence inertial range cascade. We argue that the observed dynamics is the very early manifestation of large-scale in situ nonlinear couplings that drive turbulence and heating in the solar wind.
机译：最近对太阳能​​关系的分析（立体声）成像观察已经描述了在太阳能最小条件下的年轻太阳能中的湍流开发的早期阶段。在这里，我们将该分析扩展到基于内部边界条件，偶极或磁图类型的电晕和太阳能的全局磁力学（MHD）模拟，所述偶极子或磁图型。使用尤利索和1个au观察校准模拟，并允许在良好的背景下，精确地确定Alfvén临界表面的位置，并且第一等离子体β等于单位表面。直接比较揭示了立体观测和模拟的兼容性。在模拟中计算二阶磁场结构功能的径向演进表明在几种通用克的尺度上朝向更短的各向同性条件的转变，如在40-60r_⊙的立体观察中所见。我们确认各等调化发生在第一个β统一表面附近。进一步详细阐述了基于原位太阳风湍流进化的早期阶段的解释，强调观察到的长度尺度与最终成为熟悉的湍流惯性范围级联的更小的尺度的关系。我们认为观察到的动力学是大规模的大规模出现非线性联轴器的早期表现，可在太阳风中驱动湍流和加热。

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