SCALING OF THE ELECTRON DISSIPATION RANGE OF SOLAR WIND TURBULENCE
SCALING OF THE ELECTRON DISSIPATION RANGE OF SOLAR WIND TURBULENCE
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DOI：
10.1088/0004-637x/777/1/15
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发表时间：
2013-03
期刊：
影响因子：
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通讯作者：
F. Sahraoui;S. Y. Huang;G. Belmont;M. Goldstein;A. Retinò;P. Robert;J. de Patoul
中科院分区：
文献类型：
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作者：
F. Sahraoui;S. Y. Huang;G. Belmont;M. Goldstein;A. Retinò;P. Robert;J. de Patoul
近年来，电子尺度太阳风湍流引起了人们的广泛关注。相当多的证据表明，在质子尺度附近，湍流并没有完全消散，而是继续向下级联到电子尺度。然而，磁能谱的尺度以及在这些小尺度下所涉及的等离子体模式的性质仍然没有完全确定。在这里，我们调查了在SW测量的10年的Cluster STAFF搜索线圈磁强计波形，并对频率范围[1,180]Hz的磁能谱进行了统计研究。我们发现75%的分析光谱在电子陀螺尺度ρe附近表现出断点，其次是更陡峭的幂律谱。我们表明，由于我们详细讨论的仪器限制，不能明确地确定电子断点以下的缩放。我们将我们的研究结果与其他研究的结果进行了比较，并讨论了它们对SW能量耗散的物理机制和理论建模的影响。
Electron scale solar wind (SW) turbulence has attracted great interest in recent years. Considerable evidence exists that the turbulence is not fully dissipated near the proton scale, but continues cascading down to electron scales. However, the scaling of the magnetic energy spectra as well as the nature of the plasma modes involved at those small scales are still not fully determined. Here we survey 10 yr of the Cluster STAFF search-coil magnetometer waveforms measured in the SW and perform a statistical study of the magnetic energy spectra in the frequency range [1, 180] Hz. We found that 75% of the analyzed spectra exhibit breakpoints near the electron gyroscale ρe, followed by steeper power-law-like spectra. We show that the scaling below the electron breakpoint cannot be determined unambiguously due to instrumental limitations that we discuss in detail. We compare our results to those reported in other studies and discuss their implications for the physical mechanisms involved and for theoretical modeling of energy dissipation in the SW.