Rankine–Hugoniot Relations and Magnetic Field Enhancement in Turbulent Shocks

Gedalin, Michael

doi:10.3847/1538-4357/ad0461

Cited by 7 publications

(3 citation statements)

References 31 publications

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“…Although our analysis does not depend on the validity of the R-H jump conditions, we discuss how common it is for IP shocks to comply with them. While it is generally accepted that for laminar low Mach number shocks, standard textbook R-H conditions capture the evolution of magnetic field and plasma parameters across the shock front, the situation is much more complex when the upstream medium contains some level of self-induced or preexisting population of magnetic field and plasma fluctuations (Trotta et al 2022b;Gedalin 2023;Trotta et al 2023a). The two mutually connected phenomena showing the complexity of the problem are the shock normal variability (connected to the shock rippling) and order-of-one fluctuations of the magnetic field (δB/B 0 ∼ 1) in upstream/downstream regions.…”

Section: Discussionmentioning

confidence: 99%

Turbulent Heating of Solar Wind Plasma Downstream of Magnetohydrodynamic Shocks

Pitňa,

Šafránková,

Němeček

et al. 2024

ApJ

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Interplanetary (IP) shocks are believed to play a significant role in both amplifying the background level of turbulent fluctuations and in heating the bulk solar wind (SW). This study investigates the thermodynamic properties downstream of IP shocks. We examine the temperature, density, and specific entropy changes in the shocked plasma, taking into consideration the geometric aspects of IP shock propagation within the expanding SW. Specifically, in our analysis, we account for the fact that any particular temporal range of one-point measurement may correspond to vastly different physically relevant temporal and/or spatial dimensions, such as the age of the shocked plasma and/or radial distance to the place where the plasma encountered the shock. Thus, our approach resolves the contradictions in previously reported temperature and specific entropy profiles in downstream regions and suggests that downstream regions exhibit greater turbulent heating compared to the pristine SW. This may contribute to the overall heating of the SW plasma. The paper presents a phenomenological parameter to predict specific entropy profiles and demonstrates the consistency of the proposed model with observations. We discuss the implications of these results for the thermodynamics of the SW beyond 1 au.

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Section: Discussionmentioning

confidence: 99%

Turbulent Heating of Solar Wind Plasma Downstream of Magnetohydrodynamic Shocks

Pitňa,

Šafránková,

Němeček

et al. 2024

ApJ

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“…The shock variability, particularly important for supercritical shocks, on a variety of scales (e.g., Marghitu et al 2017;Kajdič et al 2019Kajdič et al , 2021, may therefore introduce fluctuations in the decompression. Finally, as discussed in the Appendix, the decompression method makes use of the Rankine-Hugoniot jump conditions without including waves and/or turbulence (e.g., Zank et al 2002;Gedalin 2023). This technique can be further improved, in future studies, to mitigate the above limitations.…”

Section: The Shock At Parker Solar Probementioning

confidence: 99%

Properties of an Interplanetary Shock Observed at 0.07 and 0.7 au by Parker Solar Probe and Solar Orbiter

Trotta,

Larosa,

Nicolaou

et al. 2024

ApJ

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The Parker Solar Probe (PSP) and Solar Orbiter (SolO) missions opened a new observational window in the inner heliosphere, which is finally accessible to direct measurements. On 2022 September 5, a coronal mass ejection (CME)-driven interplanetary (IP) shock was observed as close as 0.07 au by PSP. The CME then reached SolO, which was radially well-aligned at 0.7 au, thus providing us with the opportunity to study the shock properties at different heliocentric distances. We characterize the shock, investigate its typical parameters, and compare its small-scale features at both locations. Using the PSP observations, we investigate how magnetic switchbacks and ion cyclotron waves are processed upon shock crossing. We find that switchbacks preserve their V–B correlation while compressed upon the shock passage, and that the signature of ion cyclotron waves disappears downstream of the shock. By contrast, the SolO observations reveal a very structured shock transition, with a population of shock-accelerated protons of up to about 2 MeV, showing irregularities in the shock downstream, which we correlate with solar wind structures propagating across the shock. At SolO, we also report the presence of low-energy (∼100 eV) electrons scattering due to upstream shocklets. This study elucidates how the local features of IP shocks and their environments can be very different as they propagate through the heliosphere.

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“…The latest development, based on the close inspection of the MMS section of the database and the corresponding shock plots, is the identification of shocks with persistent downstream fluctuations of the magnetic field in incorporation of this turbulence in the Rankine-Hugoniot relations (Gedalin, 2023a(Gedalin, , 2023b.…”

Section: Conclusion: Database Usage and Importancementioning

confidence: 99%

SHARP Shock Database

Ganushkina,

van de Kamp,

Hoppe

et al. 2024

JGR Space Physics

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Despite more than half a century of Collisionless shock (CS) research, our understanding of the processes of the shock energy dissipation into the charge particle heating and acceleration remains incomplete. To help to address the problem of the rate of the data analysis on CSs being well below of the rate of the data acquisition, an open‐source high‐level database of shocks and a centralized source of advanced tools for the purpose of analyzing shock structure and dynamics have been developed. The database is called SHARP shock database by the name of the project SHARP (Shocks: structure, AcceleRation, dissiPation) funded by the European Union's Horizon 2020 program. The SHARP shock database contains shock crossings and corresponding parameters obtained from Cluster and MMS (Magnetospheric Multiscale) missions for terrestrial bow shocks, THEMIS (Time History of Events and Macroscale Interactions during Substorms)/ARTEMIS (Acceleration, Reconnection, Turbulence and Electrodynamics of the Moon's Interaction with the Sun) missions for interplanetary shocks, and MAVEN (Mars Atmosphere and Volatile EvolutioN) and VEX (Venus Express) missions for shocks at non‐magnetized planets. The SHARP shock database can be accessed via https://sharp.fmi.fi/shock‐database/.

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Rankine–Hugoniot Relations and Magnetic Field Enhancement in Turbulent Shocks

Cited by 7 publications

References 31 publications

Turbulent Heating of Solar Wind Plasma Downstream of Magnetohydrodynamic Shocks

Turbulent Heating of Solar Wind Plasma Downstream of Magnetohydrodynamic Shocks

Properties of an Interplanetary Shock Observed at 0.07 and 0.7 au by Parker Solar Probe and Solar Orbiter

SHARP Shock Database

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