Strong Perpendicular Velocity-space Diffusion in Proton Beams Observed by Parker Solar Probe

Verniero, J. L.; Chandran, Benjamin D. G.; Larson, D. E.; Paulson, K. W.; Alterman, B. L.; Badman, S. T.; Bale, S. D.; Bonnell, J. W.; Bowen, T. A.; Wit, T. Dudok de; Kasper, J. C.; Klein, K. G.; Lichko, Emily; Livi, R.; McManus, Michael D.; Rahmati, Ali; Verscharen, Daniel; Walters, Joshua R.; Whittlesey, P. L.

doi:10.3847/1538-4357/ac36d5

Cited by 22 publications

(27 citation statements)

References 38 publications

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“…Coincident with the ion scale waves is a broadening of the beam of proton velocity distribution function (VDF) that is being termed as "hammerhead" of the proton VDF. It was also shown by [228] that these features are consistent with the expectations of quasilinear diffusion in velocity space in the presence of waves. A recent paper studies proton VDFs in the presence of cyclotron waves [229].…”

Section: Energy At Kinetic Scalessupporting

confidence: 75%

“…The transfer of energy into internal degrees of freedom has been shown to happen via wave-particle interactions, stochastic heating as well as in intermittent locations [163,185,225,233]. Distribution functions in the presence of waves show signatures expected of quasilinear diffusion in the velocity space [228,229] . Larger PVI values have been shown to associate favourably with hotter plasma, consistent with simulations as well as 1au observations [231].…”

Section: Discussionmentioning

confidence: 99%

“…PSP's state-of-the-art very high time cadence measurements in the inner heliosphere have enabled identification of various wave modes including circularly polarized waves and electrostatic waves [221][222][223][224][225][226][227]. The waves are found to last anywhere from a few seconds [221] to "wave storms" a few hours long [228]. Coincident with the ion scale waves is a broadening of the beam of proton velocity distribution function (VDF) that is being termed as "hammerhead" of the proton VDF.…”

Section: Energy At Kinetic Scalesmentioning

confidence: 99%

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Observations of Cross Scale Energy Transfer in the Inner Heliosphere by Parker Solar Probe

Parashar¹,

Matthaeus²

2022

Preprint

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The solar wind, a continuous flow of plasma from the sun, not only shapes the near Earth space environment but also serves as a natural laboratory to study plasma turbulence in conditions that are not achievable in the lab. Starting with the Mariners, for more than five decades, multiple space missions have enabled in-depth studies of solar wind turbulence. Parker Solar Probe (PSP) was launched to explore the origins and evolution of the solar wind. With its state-of-the-art instrumentation and unprecedented close approaches to the sun, PSP is starting a new era of inner heliospheric exploration. In this review we discuss observations of turbulent energy flow across scales in the inner heliosphere as observed by PSP. After providing a quick theoretical overview and a quick recap of turbulence before PSP, we discuss in detail the observations of energy at various scales on its journey from the largest scales to the internal degrees of freedom of the plasma. We conclude with some open ended questions, many of which we hope that PSP will help answer.

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Section: Energy At Kinetic Scalessupporting

confidence: 75%

Section: Discussionmentioning

confidence: 99%

Section: Energy At Kinetic Scalesmentioning

confidence: 99%

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Observations of Cross Scale Energy Transfer in the Inner Heliosphere by Parker Solar Probe

Parashar¹,

Matthaeus²

2022

Preprint

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“…Moreover, evolution of the (β p∥ , T ⊥ /T ∥ ) distributions with the system expansion also has similar elements in the solar wind and the magnetosheath (see Figures 10 and 12). Therefore, in situ measurements of the magnetosheath plasma and magnetic field characteristics can serve as a laboratory of development and relaxation of plasma instabilities, contributing significantly to local (e.g., Vech et al 2021;Verniero et al 2022) and global (e.g., Hellinger et al 2015Hellinger et al , 2019Yoon 2016) solar wind dynamics. 3.…”

Section: Discussionmentioning

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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“…( 2020b ) to “wave storms” a few hours long Verniero et al. ( 2022 ). Coincident with the ion-scale waves is a broadening of the beam of proton velocity distribution function (VDF) that is being termed as “hammerhead” of the proton VDF.…”

Section: Parker Solar Probe Observationsmentioning

confidence: 99%

Observations of cross scale energy transfer in the inner heliosphere by Parker Solar Probe

Parashar

Matthaeus

2022

Rev. Mod. Plasma Phys.

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Strong Perpendicular Velocity-space Diffusion in Proton Beams Observed by Parker Solar Probe

Cited by 22 publications

References 38 publications

Observations of Cross Scale Energy Transfer in the Inner Heliosphere by Parker Solar Probe

Observations of Cross Scale Energy Transfer in the Inner Heliosphere by Parker Solar Probe

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

Observations of cross scale energy transfer in the inner heliosphere by Parker Solar Probe

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