arXiv 1303.73942013-03astro-ph.SR

太阳风turbulence电子耗散范围的标度

Scaling of the electron dissipation range of solar wind turbulence

F. Sahraoui, S. Y. Huang, J. De Patoul, G. Belmont, M. L. Goldstein, A. Retino, P. Robert, N. Cornilleau-Wehrlin

备注：: 10 pages, submitted
DOI：: 10.1088/0004-637X/777/1/15

摘要：

电子尺度的太阳风湍流是近年来研究的热点。从星团的数据中已经给出了明确的证据，表明湍流在质子尺度附近没有完全消散，而是继续级联到电子尺度。然而，在这些小尺度的能量谱的缩放以及等离子体模式的性质仍然没有完全确定。在这里，我们调查10年的集群搜索线圈磁强计（SCM）的波形测量的太阳风和执行的磁能谱的频率范围[ $1, 180$ ]Hz的统计研究。我们发现，很大一部分的光谱表现出明确的断点附近的电子陀螺仪$ρ_e$，其次是陡峭的幂律光谱。我们表明，电子断点以下的缩放不能明确地确定，由于仪器的限制，将详细讨论。我们比较了我们的结果，最近在其他研究中报道的，并讨论了它们的含义的物理机制和理论建模的能量耗散在SW。

英文摘要：

Electron scale solar wind turbulence has attracted great interest in recent years. Clear evidences have been given from the Cluster data that turbulence is not fully dissipated near the proton scale but continues cascading down to the electron scales. However, the scaling of the 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 years of the Cluster search-coil magnetometer (SCM) waveforms measured in the solar wind and perform a statistical study of the magnetic energy spectra in the frequency range [$1, 180$]Hz. We show that a large fraction of the spectra exhibit clear breakpoints near the electon gyroscale $ρ_e$, 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 will be discussed in detail. We compare our results to recent ones reported in other studies and discuss their implication on the physical mechanisms and the theoretical modeling of energy dissipation in the SW.

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