Spectrum of kinetic plasma turbulence at 0.3-0.9 astronomical units from the Sun

0543392 - ÚFA 2022 RIV US eng J - Článek v odborném periodiku
Alexandrova, O. - Jagarlamudi, V. K. - Hellinger, Petr - Maksimovic, M. - Shprits, Y. - Mangeney, A.
Spectrum of kinetic plasma turbulence at 0.3-0.9 astronomical units from the Sun.
Physical Review E. Roč. 103, č. 6 (2021), č. článku 063202. ISSN 2470-0045. E-ISSN 2470-0053
Institucionální podpora: RVO:68378289
Klíčová slova: Solar-wind turbulence * whistler-mode waves * magnetic-field * electron scales * dissipation range * power spectra * cluster * fluctuations * anisotropy * mhd
Obor OECD: Fluids and plasma physics (including surface physics)
Impakt faktor: 2.707, rok: 2021
Způsob publikování: Omezený přístup
https://journals.aps.org/pre/abstract/10.1103/PhysRevE.103.063202

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.
Trvalý link: http://hdl.handle.net/11104/0320607