EGU26-8023, updated on 14 Mar 2026
https://doi.org/10.5194/egusphere-egu26-8023
EGU General Assembly 2026
© Author(s) 2026. This work is distributed under
the Creative Commons Attribution 4.0 License.
Poster | Tuesday, 05 May, 10:45–12:30 (CEST), Display time Tuesday, 05 May, 08:30–12:30
 
Hall X4, X4.69
Anisotropies of density and magnetic field fluctuations from inertial to kinetic scales in solar wind turbulence
Alexander Pitna1, Zdenek Nemecek1, Jana Safrankova1, Gary Zank2, Eduard Kontar3, Du Toit Strauss4, and Owen Wyn Roberts5
Alexander Pitna et al.
  • 1Charles University, Faculty of Mathematics and Physics, Department of Surface and Plasma Science, Prague, Czechia (offelius@gmail.com)
  • 2Center for Space Plasma and Aeronomic Research (CSPAR), University of Alabama in Huntsville, Huntsville, USA
  • 3School of Physics & Astronomy, University of Glasgow, Glasgow, UK
  • 4Center for Space Research, North-West University, Potchefstroom, South Africa
  • 5Department of Physics, Aberystwyth University, Aberystwyth, Wales, UK

Magnetic- and density-field fluctuations in the solar wind extend over a broad range of spatial and temporal scales. At inertial (MHD) scales, magnetic-field fluctuations are dominated by Alfvénic and/or 2D turbulence, while compressive magnetic fluctuations are associated with slow and fast MHD modes. Density fluctuations at these scales arise primarily from a mixture of entropic, slow-mode, and fast-mode contributions in the transition range near ion characteristic scales, the nature of these fluctuations changes as MHD descriptions break down and kinetic effects become important. At sub-ion scales, both magnetic-field and density fluctuations are governed by fully kinetic processes. Their coupling reflects the dominance of kinetic Alfvén wave like fluctuations, leading to enhanced compressibility and altered phase relationships between density and magnetic fields. Across all these regimes, density fluctuations—tightly linked to magnetic-field variability—play a key role in the scattering of radio waves from astrophysical sources both within and beyond the heliosphere, providing a powerful diagnostic of solar-wind turbulence across scales.

In this paper, we describe observations from two long solar wind intervals measured by the BMSW instrument onboard the Spektr-R spacecraft, which provides ion density measurements at a cadence of 32 ms. Because the Spektr-R magnetometer was not operational, we analyze magnetic-field measurements from the THEMIS-C and Wind spacecraft. The analysis of density fluctuations shows that at large (inertial) scales the fluctuations are nearly isotropic, while in the kinetic range they become strongly anisotropic. In contrast, magnetic-field fluctuations display pronounced anisotropy in both the inertial and kinetic ranges. We discuss the differing anisotropic properties of density and magnetic-field fluctuations and the complications they introduce in interpreting multi-spacecraft measurements.

How to cite: Pitna, A., Nemecek, Z., Safrankova, J., Zank, G., Kontar, E., Strauss, D. T., and Roberts, O. W.: Anisotropies of density and magnetic field fluctuations from inertial to kinetic scales in solar wind turbulence, EGU General Assembly 2026, Vienna, Austria, 3–8 May 2026, EGU26-8023, https://doi.org/10.5194/egusphere-egu26-8023, 2026.