Fast damping of ultralow frequency waves excited by interplanetary shocks in the magnetosphere

Wang, Chengrui; Rankin, R.; Zong, Qiugang

doi:10.1002/2014ja020761

Cited by 21 publications

(19 citation statements)

References 63 publications

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“…According to , possible sinks of ULF wave energy include at least three mechanisms: damping through ionospheric Joule heating, generalized Landau damping, and mode coupling. By comparing the effects of Landau damping, Joule heating, and waveguide propagation, Wang et al (2015) found that Joule heating and magnetospheric waveguide propagation are insufficient to account for the observed decay rate of ULF wave energy in this event. However, Landau damping of the wave due to driftbounce resonance with energetic ions was estimated to be higher than that provided by Joule heating (Fig.…”

Section: Growth and Damping Of Ulf Wavesmentioning

confidence: 99%

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The interaction of ultra-low-frequency pc3-5 waves with charged particles in Earth’s magnetosphere

Zong

Rankin

Zhou

2017

Rev. Mod. Plasma Phys.

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142

162

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One of the most important issues in space physics is to identify the dominant processes that transfer energy from the solar wind to energetic particle populations in Earth's inner magnetosphere. Ultra-low-frequency (ULF) waves are an important consideration as they propagate electromagnetic energy over vast distances with little dissipation and interact with charged particles via drift resonance and drift-bounce resonance. ULF waves also take part in magnetosphereionosphere coupling and thus play an essential role in regulating energy flow throughout the entire system. This review summarizes recent advances in the characterization of ULF Pc3-5 waves in different regions of the magnetosphere, including ion and electron acceleration associated with these waves.

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Section: Growth and Damping Of Ulf Wavesmentioning

confidence: 99%

“…18). Wang et al (2015) estimated that drift-bounce resonance between ULF waves and O ? ions with energies ranging from a few keV to tens of keV is sufficient to explain the rapid wave damping rates observed by Cluster on Nov 7, 2004.…”

Section: Growth and Damping Of Ulf Wavesmentioning

confidence: 99%

The interaction of ultra-low-frequency pc3-5 waves with charged particles in Earth’s magnetosphere

Zong

Rankin

Zhou

2017

Rev. Mod. Plasma Phys.

Self Cite

142

162

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“…If the majority of power is driven at the magnetopause, then this suggests that ULF waves have a long lifetime in the magnetosphere and can transit the enormous distance between the magnetopause and the 10.1029/2020JA028345 plasma torus at Io's orbit-in stark contrast with the terrestrial magnetosphere, where ULF waves have been observed to dissipate in tens of minutes (Wang et al, 2015). We can compare this to an estimate of how far fast-mode waves could penetrate into the magnetosphere over a Jovian rotation by assuming conservative ranges in the Alfvén and sound speed in the plasma sheet of 100-300 km/s (Bagenal et al, 2017;Kivelson, 2016).…”

Section: Journal Of Geophysical Research: Space Physicsmentioning

confidence: 99%

The Global Distribution of Ultralow‐Frequency Waves in Jupiter's Magnetosphere

Manners

Masters

2020

JGR Space Physics

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Jupiter's giant magnetosphere is a complex system seldom in a configuration approximating steady state, and a clear picture of its governing dynamics remains elusive. Crucial to understanding how the magnetosphere behaves on a large scale are disturbances to the system on length-scales comparable to the cavity, which are communicated by magnetohydrodynamic waves in the ultralow-frequency band (<1 mHz). In this study we used magnetometer data from multiple spacecraft to perform the first global heritage survey of these waves in the magnetosphere. To map the equatorial region, we relied on the large local-time coverage provided by the Galileo spacecraft. Flyby encounters performed by Voyager 1 and 2, Pioneer 10 and 11, and Ulysses provided local-time coverage of the dawn sector. We found several hundred events where significant wave power was present, with periods spanning ∼5-60 min. The majority of events consisted of multiple superposed discrete periods. Periods at ∼15, ∼30, and ∼40 min dominated the event-averaged spectrum, consistent with the spectra of quasi-periodic pulsations often reported in the literature. Most events were clustered in the outer magnetosphere close to the magnetopause at noon and dusk, suggesting that an external driving mechanism may dominate. The most energetic events occurred close to the planet, though more sporadically, indicating an accumulation of wave energy in the inner magnetosphere or infrequent impulsive drivers in the region. Our findings suggest that dynamics of the system at large scales is modulated by this diverse population of waves, which permeate the magnetosphere through several cavities and wave guides.

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“…At SSCs, fast‐mode magnetosonic waves launched by interplanetary shocks impinging on the magnetosphere can transfer to standing shear Alfvén waves through field line resonance (Kivelson & Southwood, ); similar excitation of global Pc5 Alfven waves has been seen even for less dramatic pressure drivers in the solar wind (Takahashi et al, ). Standing shear Alfvén waves in the ULF band can exchange their energy with charged particles efficiently through drift‐bounce resonance (Wang et al, ). Theoretical studies of drift‐bounce resonance were first carried out by Southwood and Kivelson () and evidenced by various observations (e.g., Chaston et al, ; Takahashi et al, ; Yang et al, , ).…”

Section: Introductionmentioning

confidence: 99%

Global‐Scale ULF Waves Associated With SSC Accelerate Magnetospheric Ultrarelativistic Electrons

et al. 2019

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We study electron behavior in the outer radiation belts during the 16 July 2017 storm sudden commencement (SSC), in which prompt intensification of ultrarelativistic electron fluxes was observed at around L = 4.8 by Van Allen Probe B immediately after an interplanetary shock. The electron fluxes in multiple energy channels show clear oscillations in the Pc5 frequency range, although the oscillation characteristics are quite different in different energy channels. At energies above ∼1 MeV, the oscillation periods were very close to the electron drift period, which resembles an energy spectrogram evolution expected for an energetic particle injection event and its drift echoes. At lower energies, however, the oscillation periods hardly depended on the energy: They were very close to the ultralow frequency (ULF) wave period derived from electric field measurements (about 250 s according to wavelet analysis). These complex signatures are consistent with the picture of drift resonance between electrons and short-lived ULF waves with low azimuthal wave numbers. Good agreement between the observations and numerical simulations confirms that shock-induced global-scale ULF waves can efficiently accelerate outer belt ultrarelativistic electrons up to 3.4 MeV over a time scale shorter than 1 hr.

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Fast damping of ultralow frequency waves excited by interplanetary shocks in the magnetosphere

Cited by 21 publications

References 63 publications

The interaction of ultra-low-frequency pc3-5 waves with charged particles in Earth’s magnetosphere

The interaction of ultra-low-frequency pc3-5 waves with charged particles in Earth’s magnetosphere

The Global Distribution of Ultralow‐Frequency Waves in Jupiter's Magnetosphere

Global‐Scale ULF Waves Associated With SSC Accelerate Magnetospheric Ultrarelativistic Electrons

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