Electron and ion heating by whistler turbulence: Three‐dimensional particle‐in‐cell simulations

Hughes, Randall; Gary, S. Peter; Wang, Joseph

doi:10.1002/2014gl062070

Cited by 29 publications

(29 citation statements)

References 48 publications

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“…Ions and electrons are heated by the decay of whistler turbulence observed in the solar wind [46][47][48]. Interactions of counter-propagating waves should frequently occur in the turbulence so that it is interesting to examine the collisions of two waves with different frequencies.…”

Section: Discussionmentioning

confidence: 99%

Ultrafast wave-particle energy transfer in the collapse of standing whistler waves

et al. 2019

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Efficient energy transfer from electromagnetic waves to ions has been demanded to control laboratory plasmas for various applications and could be useful to understand the nature of space and astrophysical plasmas. However, there exists a severe unsolved problem that most of the wave energy is converted quickly to electrons, but not to ions. Here, an energy conversion process to ions in overdense plasmas associated with whistler waves is investigated by numerical simulations and theoretical model. Whistler waves propagating along a magnetic field in space and laboratories often form the standing waves by the collision of counter-propagating waves or through the reflection. We find that ions in the standing whistler waves acquire a large amount of energy directly from the waves in a short timescale comparable to the wave oscillation period. Thermalized ion temperature increases in proportion to the square of the wave amplitude and becomes much higher than the electron temperature in a wide range of wave-plasma conditions. This efficient ion-heating mechanism applies to various plasma phenomena in space physics and fusion energy sciences.

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Section: Discussionmentioning

confidence: 99%

Ultrafast wave-particle energy transfer in the collapse of standing whistler waves

et al. 2019

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“…This produces large amplitude turbulence in the magnetosheath. This large amplitude turbulence can heat protons preferentially to electrons [38,39,45]. This increases proton beta more than electron beta; because of this higher β protons heat preferentially more than electrons.…”

Section: Discussionmentioning

confidence: 99%

Dependence of Kinetic Plasma Turbulence on Plasma β

Parashar

Matthaeus

Shay

2018

ApJL

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We study the effects of plasma β (ratio of plasma pressure to magnetic pressure) on the evolution of kinetic plasma turbulence using fully kinetic particle-in-cell simulations of decaying turbulence. We find that the plasma β systematically affects spectra, measures of intermittency, decay rates of turbulence fluctuations, and partitioning over different channels of energy exchange More specifically, an increase in plasma β leads to greater total heating, with proton heating preferentially more than electrons. Implications for achieving magnetosheath like temperature ratios are discussed. arXiv:1807.11371v1 [physics.space-ph] 30 Jul 2018

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“…If the interaction results in damping of the wave, then it will increase the temperature in the perpendicular direction relative to the background magnetic field (Brice, ). The interaction between the waves and the electrons can lead to a distribution different from the one that generated the waves (Chang et al, ; Hughes et al, ).…”

Section: Discussionmentioning

confidence: 99%

“…magnetic field (Brice, 1964). The interaction between the waves and the electrons can lead to a distribution different from the one that generated the waves (Chang et al, 2013;Hughes et al, 2014).…”

Section: Discussionmentioning

confidence: 99%

“…Finally, whistler mode waves have been observed in many different regions of the heliosphere, such as magnetic clouds (Moullard et al, 2001) and planetary atmospheres (Hughes et al, 2014), and they are closely linked to collisionless shocks, planetary, and interplanetary (Gary & Mellott, 1985;Lengyel-Frey et al, 1994;Walker et al, 1999). It is important to understand their properties, generation mechanisms, and the effects they have in the plasma in order to extrapolate to inaccessible regions of space.…”

Section: Discussionmentioning

confidence: 99%

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Statistical Study of the Properties of Magnetosheath Lion Roars

et al. 2018

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Lion roars are narrowband whistler wave emissions that have been observed in several environments, such as planetary magnetosheaths, the Earth's magnetosphere, the solar wind, downstream of interplanetary shocks, and the cusp region. We present measurements of more than 30,000 such emissions observed by the Magnetospheric Multiscale spacecraft with high-cadence (8,192 samples/s) search coil magnetometer data. A semiautomatic algorithm was used to identify the emissions, and an adaptive interval algorithm in conjunction with minimum variance analysis was used to determine their wave vector. The properties of the waves are determined in both the spacecraft and plasma rest frame. The mean wave normal angle, with respect to the background magnetic field (B 0 ), plasma bulk flow velocity (V b ), and the coplanarity plane (V b ×B 0 ) are 23 ∘ , 56 ∘ , and 0 ∘ , respectively. The average peak frequencies were ∼31% of the electron gyrofrequency ( ce ) observed in the spacecraft frame and ∼18% of ce in the plasma rest frame. In the spacecraft frame, ∼99% of the emissions had a frequency < ce , while 98% had a peak frequency < 0.72 ce in the plasma rest frame. None of the waves had frequencies lower than the lower hybrid frequency, . From the probability density function of the electron plasma e , the ratio between the electron thermal and magnetic pressure, ∼99.6% of the waves were observed with e < 4 with a large narrow peak at 0.07 and two smaller, but wider, peaks at 1.26 and 2.28, while the average value was ∼1.25.

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Electron and ion heating by whistler turbulence: Three‐dimensional particle‐in‐cell simulations

Cited by 29 publications

References 48 publications

Ultrafast wave-particle energy transfer in the collapse of standing whistler waves

Ultrafast wave-particle energy transfer in the collapse of standing whistler waves

Dependence of Kinetic Plasma Turbulence on Plasma β

Statistical Study of the Properties of Magnetosheath Lion Roars

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