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

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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.

Sobre autores

L. Rakhmanova

Space Research Institute of the Russian Academy of Sciences

Autor responsável pela correspondência
Email: rakhlud@gmail.com
Rússia, Moscow

M. Riazantseva

Space Research Institute of the Russian Academy of Sciences

Email: orearm@gmail.com
Rússia, Moscow

A. Khokhlachev

Space Research Institute of the Russian Academy of Sciences

Email: aleks.xaa@yandex.ru
Rússia, Moscow

Yu. Yermolaev

Space Research Institute of the Russian Academy of Sciences

Email: yermol@iki.rssi.ru
Rússia, Moscow

G. Zastenker

Space Research Institute of the Russian Academy of Sciences

Email: gzastenk@iki.rssi.ru
Rússia, Moscow

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