Visualization of rapid electron precipitation via chorus element wave–particle interactions

Ozaki, Mitsunori; Miyoshi, Yoshizumi; Hosokawa, K.; Oyama, S.; Kataoka, Ryuho; Ebihara, Yusuke; Ogawa, Y.; Kasahara, Yoshiya; Yagitani, Satoshi; Kasaba, Yasumasa; Kumamoto, Atsushi; Tsuchiya, Fuminori; Matsuda, Shoya; Katoh, Yutai; Hikishima, Mitsuru; Kurita, Satoshi; Otsuka, Yuichi; Moore, R. C.; Tanaka, Yoshimasa; Nosé, M.; Nagatsuma, Tsutomu; Нишитани, Н.; Kadokura, Akira; Connors, Martin; Inoue, Tomio; Matsuoka, A.; Shinohara, I.

doi:10.1038/s41467-018-07996-z

Cited by 40 publications

(61 citation statements)

References 55 publications

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“…Moreover, chorus waves are one of the most important loss mechanisms of plasma sheet electrons via pitch angle scattering (e.g., Horne et al, ). The scattered electrons into the upper atmosphere could then generate microbursts (e.g., Breneman et al, ; Nakamura et al, ; Shumko et al, ), pulsating aurora (e.g., W. Li et al, ; Nishimura et al, ; Nishimura, Bortnik, Li, Thorne, Lyons, et al, ; Nishimura, Bortnik, Li, Thorne, Chen, et al, ; Ozaki et al, , ), and diffuse aurora (e.g., Ni et al, ; Thorne et al, ).…”

Section: Introductionmentioning

confidence: 99%

“…At a higher L shell, that is, L ~ 11, Agapitov et al () showed a case with a larger scale size of chorus element, around 3,000 km, using Time History of Events and Macroscale Interactions during Substorms (THEMIS) observations. Moreover, the scale size of chorus waves is estimated by mapping the size of microburst and pulsating aurora onto the equatorial plane (e.g., Breneman et al, ; Nishimura, Bortnik, Li, Thorne, Lyons, et al, ; Nishimura, Bortnik, Li, Thorne, Chen, et al, ; Ozaki et al, , ; Shumko et al, ). On the nightside at L ~ 8, the latitudinal (longitudinal) size of pulsating aurora is found to be a few tens (hundreds) kilometers, which is roughly 3,000–7,000 km when mapping onto the equatorial plane (Nishimura, Bortnik, Li, Thorne, Chen, et al, ).…”

Section: Introductionmentioning

confidence: 99%

“…Li et al, 2007;Li, Mourenas, et al, 2014;Li, Thorne, et al, 2014;Ma et al, 2018;Meredith et al, 2003;Shen et al, 2017;Thorne et al, 2013;Tu et al, 2014;Turner et al, 2019;Xiao et al, 2014). Moreover, chorus waves are one of the most important loss mechanisms of plasma sheet electrons via pitch angle scattering (e.g., Horne et al, 2003 could then generate microbursts (e.g., Breneman et al, 2017;Nakamura et al, 2000;Shumko et al, 2018), pulsating aurora (e.g., W. Li et al, 2012;Nishimura et al, 2010;Nishimura, Bortnik, Li, Thorne, Chen, et al, 2011;Ozaki et al, 2018Ozaki et al, , 2019, and diffuse aurora (e.g., Ni et al, 2008;Thorne et al, 2010).…”

Section: Introductionmentioning

confidence: 99%

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Statistical Analysis of Transverse Size of Lower Band Chorus Waves Using Simultaneous Multisatellite Observations

Shen

et al. 2019

Geophysical Research Letters

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Chorus waves are known to accelerate or scatter energetic electrons via quasi‐linear or nonlinear wave‐particle interactions in the Earth's magnetosphere. In this letter, by taking advantage of simultaneous observations of chorus waveforms from at least a pair of probes among Van Allen Probes and/or Time History of Events and Macroscale Interactions during Substorms (THEMIS) missions, we statistically calculate the transverse size of lower band chorus wave elements. The average size of lower band chorus wave element is found to be ~315±32 km over L shells of ~5–6. Furthermore, our results suggest that the scale size of lower band chorus tends to be (1) larger at higher L shells; (2) larger at higher magnetic latitudes, especially on the dayside; and (3) larger in the azimuthal direction than in the radial direction. Our findings are crucial to quantify wave‐particle interaction process, particularly the nonlinear interactions between chorus and energetic electrons.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Statistical Analysis of Transverse Size of Lower Band Chorus Waves Using Simultaneous Multisatellite Observations

Shen

et al. 2019

Geophysical Research Letters

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“…Most statistical studies rely primarily on time-averaged spectral data, which obscures the true amplitude of short-lived, large-amplitude wave packets. Ozaki et al (2019) observed that large (hundreds of picoteslas), isolated chorus wave packets directly caused auroral flashes seen from ground stations. These large-amplitude whistler mode waves interact differently with electrons than their lower-amplitude counterparts, resulting in trapping, and rapid energization or de-energization, and pitch angle scattering (Bortnik et al, 2008;Cattell et al, 2008;Kellogg et al, 2010;Kersten et al, 2011;Omura et al, 2008).…”

Section: Introductionmentioning

confidence: 99%

Statistical Distribution of Whistler Mode Waves in the Radiation Belts With Large Magnetic Field Amplitudes and Comparison to Large Electric Field Amplitudes

et al. 2019

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We present a statistical analysis with 100% duty cycle and non‐time‐averaged amplitudes of the prevalence and distribution of high‐amplitude >50‐pT whistler mode waves in the outer radiation belt using 5 years of Van Allen Probes data. Whistler mode waves with high magnetic field amplitudes are most common above L=4.5 and between magnetic local time of 0–14 where they are present approximately 1–6% of the time. During high geomagnetic activity, high‐amplitude whistler mode wave occurrence rises above 25% in some regions. The dayside population are more common during quiet or moderate geomagnetic activity and occur primarily >5° from the magnetic equator, while the night‐to‐dawn population are enhanced during active times and are primarily within 5° of the magnetic equator. These results are different from the distribution of electric field peaks discussed in our previous paper covering the same time period and spatial range. Our previous study found large‐amplitude electric field peaks were common down to L=3.5 and were largely absent from afternoon and near noon. The different distribution of large electric and magnetic field amplitudes implies that the low‐L component of whistler mode waves observed previously are primarily highly oblique, while the dayside and high‐L populations are primarily field aligned. These results have important implications for modeling radiation belt particle interactions with chorus, as large‐amplitude waves interact nonlinearly with electrons, resulting in rapid energization, de‐energization, or pitch angle scattering. This also may provide clues regarding the mechanisms which can cause significant whistler mode wave growth up to more than 100 times the average wave amplitude.

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“…Chorus emissions are generated near the equatorial plane in the magnetosphere by high-energy electrons with temperature anisotropy (e.g., Kennel & Petschek, 1966;LeDocq et al, 1998;Santolik et al, 2003). Chorus emissions are known to accelerate electrons to relativistic energy levels in the outer radiation belt and scatter them at the electron pitch angle through wave-particle interactions (e.g., Horne et al, 2007;Kasahara et al, 2018;Li et al, 2014;Meredith et al, 2003;Miyoshi et al, 2015;Ozaki et al, 2019). QP emissions are categorized as discrete electromagnetic waves with QP intensity enhancement on a time scale of ∼10-400 s (e.g., Manninen et al, 2014Manninen et al, , 2018Nemec et al, 2016;Titova et al, 2015).…”

Section: Introductionmentioning

confidence: 99%

Longitudinal Extent of Magnetospheric ELF/VLF Waves using Multipoint PWING Ground Stations at Subauroral Latitudes

et al. 2019

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Magnetospheric extremely low frequency/very low frequency (ELF/VLF) waves are plasma waves emitted from high-energy electrons in the magnetosphere. These waves have received much attention, as they contribute to the acceleration and loss of relativistic electrons in the radiation belts through wave-particle interactions. The longitudinal extent of ELF/VLF waves has not been well-understood, although the extent is important in quantitative evaluation of relativistic electron variations. In this study, we analyzed data from continuous ground-based simultaneous observations of ELF/VLF waves over a 2-month period in November and December of 2017, using six loop antennas located at roughly equal intervals around the north geomagnetic pole at ∼ 60 • magnetic latitudes. We estimated the longitudinal extent of magnetospheric ELF/VLF waves based on their occurrence rate. Our results showed that the ELF/VLF wave occurrence rate differed by twofold to threefold, depending on the longitudes of the observation sites. We explain this difference in terms of longitudinal differences in the ionosphere's magnetic field intensity, possibly due to the electron loss that occurs during the bounce motion at longitudes of small magnetic field intensity. Based on our statistical analysis, we estimated the typical longitudinal extent of ELF/VLF waves as ∼ 76 • . Time series analysis results showed that the large longitudinal extent of the ELF/VLF waves occurs frequently during the main phase of geomagnetic storms and is also associated with substorms represented by the auroral electrojet index.Hiss emissions are categorized as continuous electromagnetic waves with broadband and non-structured features (Hayakawa et al., 1986). The generation mechanism has been considered to be a mixture of propagating and reflecting chorus waves in the magnetosphere (e.g.

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Visualization of rapid electron precipitation via chorus element wave–particle interactions

Cited by 40 publications

References 55 publications

Statistical Analysis of Transverse Size of Lower Band Chorus Waves Using Simultaneous Multisatellite Observations

Statistical Analysis of Transverse Size of Lower Band Chorus Waves Using Simultaneous Multisatellite Observations

Statistical Distribution of Whistler Mode Waves in the Radiation Belts With Large Magnetic Field Amplitudes and Comparison to Large Electric Field Amplitudes

Longitudinal Extent of Magnetospheric ELF/VLF Waves using Multipoint PWING Ground Stations at Subauroral Latitudes

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