Decay of Space Plasma Turbulence Downstream of Bow Shocks: MMS Magnetosheath Unbiased Campaign Observations
13 affiliations
- 1University of Murcia
- 2Universitat de les Illes Balears (UIB)
- 3Institute of Applied Computing & Community Code (IAC3)
- 4Astronomical Institute of the Czech Republic
- 5Institute of Atmospheric Physics of the Czech Academy of Sciences, Prague,
- 6INAF—Osservatorio Astrofísico di Arcetri
- 7University of Florence
- 8Istituto per la Scienza e Tecnologia dei Plasmi
- 9KTH Royal Institute of Technology
- 10University of Delaware
- 11Northumbria University
- 12Laboratory for Atmospheric and Space Physics
- 13Instituto di Astrofísica e Planetologia Spaziali
Abstract
Turbulence properties in the solar wind change with increasing heliospheric distance. Observations from different missions have shown how spectral indices converge toward an f −5/3 spectrum in the inertial range as the solar wind reaches 1 au and how the cascade rate decays as the plasma moves away from the Sun. We evaluate whether these properties display similar trends in a smaller astrophysical system, that of a planetary magnetosheath. Using data from the 2023 Magnetospheric Multiscale (MMS) unbiased magnetosheath campaign, we determine the evolution of the spectral indices and the cascade rate along 15 inbound magnetosheath crossings. WIND observations were permitted to monitor the state of the solar wind during the campaign and allowed to study the impact of the upstream plasma conditions on the evolution of the cascade rate downstream from the bow shock. Our results show an increase of the cascade rate between 2 and 3 orders of magnitude after the plasma crosses the bow shock into the magnetosheath. Once in the magnetosheath, turbulence develops with increasing distance to the bow shock in a way similar to solar wind observations, despite the smaller size of the system. Incompressible Hall magnetohydrodynamics (MHD) scaling-law estimates of the cascade rate show a clear power-law decay of the cascade rate in the magnetosheath, particularly for the cases with upstream slow wind. This suggests that the way energy is injected into the system plays a role in the decay of turbulence as the plasma moves away from the bow shock.
Versions
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BibTeX
@article{montagudcamps2026decay,
title = {{Decay of Space Plasma Turbulence Downstream of Bow Shocks: MMS Magnetosheath Unbiased Campaign Observations}},
author = {Victor Montagud-Camps and Petr Hellinger and Sergio Toledo-Redondo and Andrea Verdini and Luca Sorriso-Valvo and Francesco Pecora and Julia E. Stawarz and Alexandros Chasapis and Emanuele Papini and Inmaculada F. Albert and Aida Castilla},
journal = {The Astrophysical Journal},
year = {2026},
month = sep,
doi = {10.3847/1538-4357/ae9ebc},
url = {https://iopscience.iop.org/article/10.3847/1538-4357/ae9ebc},
note = {CC BY 4.0},
}
RIS
TY - JOUR
TI - Decay of Space Plasma Turbulence Downstream of Bow Shocks: MMS Magnetosheath Unbiased Campaign Observations
AU - Victor Montagud-Camps
AU - Petr Hellinger
AU - Sergio Toledo-Redondo
AU - Andrea Verdini
AU - Luca Sorriso-Valvo
AU - Francesco Pecora
AU - Julia E. Stawarz
AU - Alexandros Chasapis
AU - Emanuele Papini
AU - Inmaculada F. Albert
AU - Aida Castilla
PY - 2026
DA - 2026/09/30
JO - The Astrophysical Journal
DO - 10.3847/1538-4357/ae9ebc
UR - https://iopscience.iop.org/article/10.3847/1538-4357/ae9ebc
AB - Turbulence properties in the solar wind change with increasing heliospheric distance. Observations from different missions have shown how spectral indices converge toward an f −5/3 spectrum in the inertial range as the solar wind reaches 1 au and how the cascade rate decays as the plasma moves away from the Sun. We evaluate whether these properties display similar trends in a smaller astrophysical system, that of a planetary magnetosheath. Using data from the 2023 Magnetospheric Multiscale (MMS) unbiased magnetosheath campaign, we determine the evolution of the spectral indices and the cascade rate along 15 inbound magnetosheath crossings. WIND observations were permitted to monitor the state of the solar wind during the campaign and allowed to study the impact of the upstream plasma conditions on the evolution of the cascade rate downstream from the bow shock. Our results show an increase of the cascade rate between 2 and 3 orders of magnitude after the plasma crosses the bow shock into the magnetosheath. Once in the magnetosheath, turbulence develops with increasing distance to the bow shock in a way similar to solar wind observations, despite the smaller size of the system. Incompressible Hall magnetohydrodynamics (MHD) scaling-law estimates of the cascade rate show a clear power-law decay of the cascade rate in the magnetosheath, particularly for the cases with upstream slow wind. This suggests that the way energy is injected into the system plays a role in the decay of turbulence as the plasma moves away from the bow shock.
SN - 0004-637X
SN - 1538-4357
ER -