Evidence for Iroshnikov-Kraichnan-type turbulence in the solar wind upstream of interplanetary traveling shocks

被引：19

作者：

Bamert, K. ^{[1
]}

Kallenbach, R. ^{[1
,2
,3
]}

le Roux, J. A. ^{[2
]}

Hilchenbach, M. ^{[3
]}

Smith, C. W. ^{[4
,5
]}

Wurz, P. ^{[1
]}

机构：

[1] Univ Bern, Inst Phys, Bern, Switzerland

[2] Univ Calif Riverside, Inst Geophys & Planetary Phys, Riverside, CA 92521 USA

[3] Max Planck Inst Sonnensyst Forsch, Katlenburg Lindau, Germany

[4] Univ New Hampshire, Dept Phys, Durham, NH 03824 USA

[5] Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2008年 / 675卷 / 01期

关键词：

acceleration of particles; MHD; shock waves; solar wind; Sun : coronal mass ejections (CMEs); turbulence;

D O I：

10.1086/529491

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We analyze suprathermal ions and plasma wave spectra upstream of interplanetary shocks driven by coronal mass ejection events. In particular, we analyze the competition between two processes: (1) the upstream wave generation by suprathermal protons accelerated at the shock, and (2) the cascading of wave energy in the inertial range of solar wind turbulence. We derive the cascading timescale from the comparison of particle and turbulent wave spectra with theory and conclude that amplified solar wind turbulence upstream of interplanetary traveling shocks is better described by Iroshnikov-Kraichnan-type rather than Kolmogorov-type wave diffusion.

引用

页码：L45 / L48

页数：4

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