Role of middle-scale solar wind structures in the turbulence development behind the bow shock

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Abstract

Present study estimates contribution of the middle-scale solar wind structures (variations which are registered by a spacecraft during ~10 min intervals) in the turbulence development in the transition region behind the bow shock. The analysis is based on simultaneous measurements of plasma and/or magnetic field parameters in the solar wind, in the dayside magnetosheath and at the flanks. The study adopts measurements by Wind, THEMIS and Spektr-R spacecraft. Properties of magnetic field and ion flux fluctuation spectra are analyzed in the frequency range 0.01-4 Hz, which corresponds to transition from MHD to kinetic scales. The dynamics of turbulence properties in the magnetosheath is governed by large-scale disturbances while structures with smaller scales have effect during absence of large-scale structures.

About the authors

L. S. Rakhmanova

Space Research Institute of the Russian Academy of Sciences

Author for correspondence.
Email: rakhlud@gmail.com
Russian Federation, Moscow

M. O. Riazantseva

Space Research Institute of the Russian Academy of Sciences

Email: orearm@gmail.com
Russian Federation, Moscow

A. A. Khokhlachev

Space Research Institute of the Russian Academy of Sciences

Email: aleks.xaa@yandex.ru
Russian Federation, Moscow

Yu. I. Yermolaev

Space Research Institute of the Russian Academy of Sciences

Email: yermol@iki.rssi.ru
Russian Federation, Moscow

G. N. Zastenker

Space Research Institute of the Russian Academy of Sciences

Email: gzastenk@iki.rssi.ru
Russian Federation, Moscow

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