Number of the records: 1
Spectrum of kinetic plasma turbulence at 0.3-0.9 astronomical units from the Sun
- 1.
SYSNO ASEP 0543392 Document Type J - Journal Article R&D Document Type Journal Article Subsidiary J Článek ve WOS Title Spectrum of kinetic plasma turbulence at 0.3-0.9 astronomical units from the Sun Author(s) Alexandrova, O. (FR)
Jagarlamudi, V. K. (FR)
Hellinger, Petr (UFA-U) RID, ORCID
Maksimovic, M. (FR)
Shprits, Y. (DE)
Mangeney, A. (FR)Number of authors 6 Article number 063202 Source Title Physical Review E. - : American Physical Society - ISSN 2470-0045
Roč. 103, č. 6 (2021)Number of pages 9 s. Language eng - English Country US - United States Keywords Solar-wind turbulence ; whistler-mode waves ; magnetic-field ; electron scales ; dissipation range ; power spectra ; cluster ; fluctuations ; anisotropy ; mhd Subject RIV BL - Plasma and Gas Discharge Physics OECD category Fluids and plasma physics (including surface physics) Method of publishing Limited access Institutional support UFA-U - RVO:68378289 UT WOS 000657177000007 EID SCOPUS 85108077108 DOI 10.1103/PhysRevE.103.063202 Annotation We investigate spectral properties of turbulence in the solar wind that is a weakly collisional astrophysical plasma, accessible to in situ observations. Using the Helios search coil magnetometer measurements in the fast solar wind, in the inner heliosphere, we focus on properties of the turbulent magnetic fluctuations at scales smaller than the ion characteristic scales, the so-called kinetic plasma turbulence. At such small scales, we show that magnetic power spectra between 0.3 and 0.9 AU from the Sun have a generic shape similar to f(-8/3) exp (-f/f(d)), where the dissipation frequency f(d) is correlated with the Doppler shifted frequency f(rho e) of the electron Larmor radius. This behavior is statistically significant: all the observed kinetic spectra are well described by this model, with f(d) = f(rho e)/1.8. Our results indicate that the electron gyroradius plays the role of the dissipation scale and marks the end of the electromagnetic cascade in the solar wind. Workplace Institute of Atmospheric Physics Contact Kateřina Adamovičová, adamovicova@ufa.cas.cz, Tel.: 272 016 012 ; Kateřina Potužníková, kaca@ufa.cas.cz, Tel.: 272 016 019 Year of Publishing 2022 Electronic address https://journals.aps.org/pre/abstract/10.1103/PhysRevE.103.063202
Number of the records: 1