2020/07/31 by Owen Wyn Roberts, Rumi Nakamura, Klaus Torkar +10
Physics and Astronomy · #Astro and Planetary Science #Ionosphere and magnetosphere dynamics #Kinetic energy #Noise (video) #Plasma #Range (aeronautics) #Solar and Space Plasma Dynamics #Solar wind #Spacecraft #Spectral density #Turbulence #physics.plasm-ph #physics.space-ph
paper · pdf · doi:10.3847/1538-4365/abb45d
Accepted to APJS
openalex created_date 2020/07/23 · arxiv created 2020/09/01 · openalex publication_date 2020/10/01 · arxiv updated 2020/10/21 · openalex updated_date 2026/08/05
Abstract Compressive plasma turbulence is investigated at sub-ion scales in the solar wind using both the Fast Plasma Investigation (FPI) instrument on the Magnetospheric MultiScale mission (MMS), as well as using calibrated spacecraft potential data from the Spin Plane Double Probe (SDP) instrument. The data from FPI allow the sub-ion scale region ( f sc ≳ 1 Hz) to be investigated before the instrumental noise becomes significant at a spacecraft frame frequency of f sc ≈ 3 Hz. Whereas the calibrated spacecraft potential allows a measurement up to f sc ≈ 40 Hz. In this work, we give a detailed description of density estimation in the solar wind using the spacecraft potential measurement from the SDP instrument on MMS. Several intervals of solar wind plasma have been processed using the methodology described and are made available. One of the intervals is investigated in more detail and the power spectral density of the compressive fluctuations is measured from the inertial range to the sub-ion range. The morphology of the density spectra can be explained by either a cascade of Alfvén waves and slow waves at large scales and kinetic Alfvén waves at sub-ion scales or more generally by the Hall effect. Using electric field measurements, the two hypotheses are discussed.