Dependence of Solar Wind Proton Temperature on the Polarization Properties of Alfvénic Fluctuations at Ion-kinetic Scales

Woodham, L. D.; Wicks, Robert T.; Verscharen, Daniel; TenBarge, Jason; Howes, G. G.

doi:10.3847/1538-4357/abed51

Cited by 12 publications

(6 citation statements)

References 135 publications

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“…Although this applies both inside and outside the CS, it occurs mainly along the CS boundaries (only the core population at the CS layers exceeds the firehose instability; this is more evident during the first passage). In these time intervals, the system can drive parallel fast-mode waves with a polarization opposite from ICWs in the plasma frame (Woodham et al 2021). A further in situ analysis of these fast-mode waves, however, is beyond the scope of the present work though, which focuses primarily on ICWs, whose presence is evidenced by Figure 5 and whose importance is related to their possible contribution in the coronal plasma heating mechanisms discussed in Section 1.…”

Section: Onset Of Icws Along the Turbulent Csmentioning

confidence: 90%

Does Turbulence along the Coronal Current Sheet Drive Ion Cyclotron Waves?

Telloni

Zank

Adhikari

et al. 2023

ApJ

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Evidence for the presence of ion cyclotron waves (ICWs), driven by turbulence, at the boundaries of the current sheet is reported in this paper. By exploiting the full potential of the joint observations performed by Parker Solar Probe and the Metis coronagraph on board Solar Orbiter, local measurements of the solar wind can be linked with the large-scale structures of the solar corona. The results suggest that the dynamics of the current sheet layers generates turbulence, which in turn creates a sufficiently strong temperature anisotropy to make the solar-wind plasma unstable to anisotropy-driven instabilities such as the Alfvén ion cyclotron, mirror-mode, and firehose instabilities. The study of the polarization state of high-frequency magnetic fluctuations reveals that ICWs are indeed present along the current sheet, thus linking the magnetic topology of the remotely imaged coronal source regions with the wave bursts observed in situ. The present results may allow improvement of state-of-the-art models based on the ion cyclotron mechanism, providing new insights into the processes involved in coronal heating.

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Section: Onset Of Icws Along the Turbulent Csmentioning

confidence: 90%

Does Turbulence along the Coronal Current Sheet Drive Ion Cyclotron Waves?

Telloni

Zank

Adhikari

et al. 2023

ApJ

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“…For the waves and turbulence in the solar wind, their observations from a single spacecraft are significantly affected by the sampling effect (e.g., Fredricks & Coroniti 1976;Howes & Quataert 2010;Horbury et al 2012;Bowen et al 2020b; Woodham et al 2021). Consequently, this sampling effect is one key factor determining the occurrence rate of the observed ion-scale waves (Bowen et al 2020b).…”

Section: The Sampling Effectmentioning

confidence: 99%

The Radial Distribution of Ion-scale Waves in the Inner Heliosphere

Liu

Zhao

Wang

et al. 2023

ApJ

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Determining the mechanism responsible for plasma heating and particle acceleration is a fundamental problem in the study of the heliosphere. Due to efficient wave–particle interactions of ion-scale waves with charged particles, these waves are widely believed to be a major contributor to ion energization, and their contribution considerably depends on the wave occurrence rate. By analyzing the radial distribution of quasi-monochromatic ion-scale waves observed by the Parker Solar Probe, this work shows that the wave occurrence rate is significantly enhanced in the near-Sun solar wind, specifically 21%–29% below 0.3 au, in comparison to 6%–14% beyond 0.3 au. The radial decrease of the wave occurrence rate is not only induced by the sampling effect of a single spacecraft detection, but also by the physics relating to the wave excitation, such as the enhanced ion beam instability in the near-Sun solar wind. This work also shows that the wave normal angle θ, the absolute value of ellipticity ϵ, the wave frequency f normalized by the proton cyclotron frequency f cp, and the wave amplitude δ B normalized by the local background magnetic field B 0 slightly vary with the radial distance. The median values of θ, ∣ϵ∣, f, and δ B are about 9°, 0.73, 3f cp, and 0.01B 0, respectively. Furthermore, this study proposes that the wave mode natures of the observed left-handed and right-handed polarized waves correspond to the Alfvén ion cyclotron mode wave and the fast magnetosonic whistler mode wave, respectively.

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“…However, there is no strong damping of density fluctuations at the low-frequency range in the simulation results. Observations and simulations show that the fluctuation intensity evolves differently for different frequency ranges, i.e., there is a spectrum shape change around ion-kinetic scales likely supported by local kinetic processes (e.g., plasma instabilities and Landau damping; see Hellinger et al 2015Hellinger et al , 2019Woodham et al 2021a).…”

Section: Properties Of Magnetic Field and Plasma Fluctuationsmentioning

confidence: 99%

“…A complex mixture of effects-nonlinear Alfvén wave dynamics on fluid scales, various kinetic instabilities on ion scales, and the solar wind expansion-depend also on solar wind structure and internal correlations in the solar wind (e.g., Perrone et al 2019a, 2019b, andreferences therein), where plasma flow speed (e.g., Bruno et al 2014a;Verscharen et al 2021) and plasma beta (e.g., Duan et al 2020;Woodham et al 2021a) control many fluctuation properties. The wide range of temporal and spatial scales as well as parameter ranges involved complicate their understanding via numerical simulation and investigations with spacecraft observations.…”

Section: Introductionmentioning

confidence: 99%

Ion Kinetics of Plasma Flows: Earth's Magnetosheath versus Solar Wind

Artemyev

Shi

Lin

et al. 2022

ApJ

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Revealing the formation, dynamics, and contribution to plasma heating of magnetic field fluctuations in the solar wind is an important task for heliospheric physics and for a general plasma turbulence theory. Spacecraft observations in the solar wind are limited to spatially localized measurements, so that the evolution of fluctuation properties with solar wind propagation is mostly studied via statistical analyses of data sets collected by different spacecraft at various radial distances from the Sun. In this study we investigate the evolution of turbulence in the Earth’s magnetosheath, a plasma system sharing many properties with the solar wind. The near-Earth space environment is being explored by multiple spacecraft missions, which may allow us to trace the evolution of magnetosheath fluctuations with simultaneous measurements at different distances from their origin, the Earth’s bow shock. We compare ARTEMIS and Magnetospheric Multiscale (MMS) Mission measurements in the Earth magnetosheath and Parker Solar Probe measurements of the solar wind at different radial distances. The comparison is supported by three numerical simulations of the magnetosheath magnetic and plasma fluctuations: global hybrid simulation resolving ion kinetic and including effects of Earth’s dipole field and realistic bow shock, hybrid and Hall-MHD simulations in expanding boxes that mimic the magnetosheath volume expansion with the radial distance from the dayside bow shock. The comparison shows that the magnetosheath can be considered as a miniaturized version of the solar wind system with much stronger plasma thermal anisotropy and an almost equal amount of forward and backward propagating Alfvén waves. Thus, many processes, such as turbulence development and kinetic instability contributions to plasma heating, occurring on slow timescales and over large distances in the solar wind, occur more rapidly in the magnetosheath and can be investigated in detail by multiple near-Earth spacecraft.

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Dependence of Solar Wind Proton Temperature on the Polarization Properties of Alfvénic Fluctuations at Ion-kinetic Scales

Cited by 12 publications

References 135 publications

Does Turbulence along the Coronal Current Sheet Drive Ion Cyclotron Waves?

Does Turbulence along the Coronal Current Sheet Drive Ion Cyclotron Waves?

The Radial Distribution of Ion-scale Waves in the Inner Heliosphere

Ion Kinetics of Plasma Flows: Earth's Magnetosheath versus Solar Wind

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