太阳风在1 au处的低频间歇性与结构
Low-frequency Intermittency and Structures in the Solar Wind at 1 au
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中文总结 AI 辅助
本研究利用Wind和ACE卫星20余年数据，发现太阳风磁场峰度在相关尺度以上仍保持超高斯，证明大尺度间歇性存在，可能源于太阳风流混合与非平稳驱动。
中文摘要 AI 辅助
太阳风中的间歇性通常在惯性范围和耗散范围内进行研究，在这些范围内，尺度相关的磁场分布随着尺度的减小而变得越来越非高斯，直到耗散变得重要。相反，在大尺度上是否恢复高斯性仍不清楚。为了解决这一问题，我们利用NASA的Wind和ACE航天器超过二十年的原位观测数据，系统地检查了从1分钟到1年的尺度上的磁场增量峰度。我们发现，尽管峰度在相关尺度附近趋向于高斯值3，但在更大尺度上通常保持升高（超高斯）。峰度也随时间显著变化，在高太阳活动阶段出现明显的超高斯区间，而亚高斯区间主要出现在径向分量中且较为零星。这些结果为太阳风中的大尺度间歇性提供了证据，这种间歇性可能源于不同太阳风流混合以及太阳源的非平稳驱动。
英文摘要
Intermittency in the solar wind is commonly studied within the inertial and dissipative ranges, where scale-dependent magnetic field distributions become increasingly non-Gaussian toward smaller scales until dissipation becomes important. Conversely, whether Gaussianity is recovered at large scales remains unclear. To address this, we systematically examine magnetic field increment kurtosis over scales from 1 minute to 1 year using more than two decades of in situ observations from NASA's Wind and ACE spacecraft. We find that although kurtosis tends toward Gaussian value of 3 near the correlation scales, it generally remains elevated (super-Gaussian) at larger scales. Kurtosis also varies substantially over time, with pronounced super-Gaussian intervals during high solar activity phases and sporadic sub-Gaussian intervals primarily in the radial component. These results provide evidence for large-scale intermittency in the solar wind, potentially arising from mixing of different solar wind streams and nonstationary driving of solar sources.
发表机构
- Department of Physics and Astronomy, University of Delaware（特拉华大学物理与天文学系）
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