SCALING OF THE ELECTRON DISSIPATION RANGE OF SOLAR WIND TURBULENCE

被引：145

作者：

Sahraoui, F. ^{[1
]}

Huang, S. Y. ^{[2
]}

Belmont, G. ^{[1
]}

Goldstein, M. L. ^{[3
]}

Retino, A. ^{[1
]}

Robert, P. ^{[1
]}

De Patoul, J. ^{[1
]}

机构：

[1] UPMC, CNRS, Ecole Polytech, Lab Phys Plasmas, F-92120 Palaiseau, France

[2] Wuhan Univ, Sch Elect & Informat, Wuhan 430072, Peoples R China

[3] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

来源：

ASTROPHYSICAL JOURNAL | 2013年 / 777卷 / 01期

关键词：

plasmas; solar wind; turbulence; WEAKLY COLLISIONAL PLASMAS; CLUSTER MISSION; SCALES; FLUCTUATIONS; SPECTRUM; CASCADE; AU;

D O I：

10.1088/0004-637X/777/1/15

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 rho 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 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.

引用

页数：11

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