Quantification of Energetic Electron Precipitation Driven by Plume Whistler Mode Waves, Plasmaspheric Hiss, and Exohiss

Li, W.; Shen, Xiaochen; Ma, Q.; Capannolo, L.; Shi, Run; Redmon, R. J.; Rodriguez, J. V.; Reeves, G. D.; Kletzing, C. A.; Kurth, W. S.; Hospodarsky, G. B.

doi:10.1029/2019gl082095

Cited by 41 publications

(63 citation statements)

References 59 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Whistler mode waves are often observed in plasmaspheric plumes (Chan & Holzer, 1976;Hayakawa et al, 1986;Li et al, 2019;Shi et al, 2019;Su et al, 2018;Tsurutani et al, 2015), which are composed of plasma…”

Section: 1029/2018ja025940mentioning

confidence: 99%

Earth's Van Allen Radiation Belts: From Discovery to the Van Allen Probes Era

2019

Self Cite

View full text Add to dashboard Cite

Discovery of the Earth's Van Allen radiation belts by instruments flown on Explorer 1 in 1958 was the first major discovery of the Space Age. The observation of distinct inner and outer zones of trapped megaelectron volt (MeV) particles, primarily protons at low altitude and electrons at high altitude, led to early models for source and loss mechanisms including Cosmic Ray Albedo Neutron Decay for inner zone protons, radial diffusion for outer zone electrons and loss to the atmosphere due to pitch angle scattering. This scattering lowers the mirror altitude for particles in their bounce motion parallel to the Earth's magnetic field until they suffer collisional loss. A view of the belts as quasi‐static inner and outer zones of energetic particles with different sources was modified by observations made during the Solar Cycle 22 maximum in solar activity over 1989–1991. The dynamic variability of outer zone electrons was measured by the Combined Radiation Release and Effects Satellite launched in July 1990. This variability is caused by distinct types of heliospheric structure that vary with the solar cycle. The launch of the twin Van Allen Probes in August 2012 has provided much longer and more comprehensive measurements during the declining phase of Solar Cycle 24. Roughly half of moderate geomagnetic storms, determined by intensity of the ring current carried mostly by protons at hundreds of kiloelectron volts, produce an increase in trapped relativistic electron flux in the outer zone. Mechanisms for accelerating electrons of hundreds of electron volts stored in the tail region of the magnetosphere to MeVenergies in the trapping region are described in this review: prompt and diffusive radial transport and local acceleration driven by magnetospheric waves. Such waves also produce pitch angle scattering loss, as does outward radial transport, enhanced when the magnetosphere is compressed. While quasilinear simulations have been used to successfully reproduce many essential features of the radiation belt particle dynamics, nonlinear wave‐particle interactions are found to be potentially important for causing more rapid particle acceleration or precipitation. The findings on the fundamental physics of the Van Allen radiation belts potentially provide insights into understanding energetic particle dynamics at other magnetized planets in the solar system, exoplanets throughout the universe, and in astrophysical and laboratory plasmas. Computational radiation belt models have improved dramatically, particularly in the Van Allen Probes era, and assimilative forecasting of the state of the radiation belts has become more feasible. Moreover, machine learning techniques have been developed to specify and predict the state of the Van Allen radiation belts. Given the potential Space Weather impact of radiation belt variability on technological systems, these new radiation belt models are expected to play a critical role in our technological society in the future as much as meteorological models do today.

show abstract

Section: 1029/2018ja025940mentioning

confidence: 99%

Earth's Van Allen Radiation Belts: From Discovery to the Van Allen Probes Era

2019

Self Cite

View full text Add to dashboard Cite

show abstract

“…This work focuses on plasmaspheric hiss, defined here as hiss found within the plasmasphere at frequencies between 150 Hz and

\sim

2 kHz. Other hiss types will be parameterized in future work, including plume hiss (Li et al, ), low‐frequency hiss (Li et al, ), lightning hiss (Meredith et al, ), and exohiss (Zhu et al, , ). By building a wave model for each hiss type separately, they can be included or excluded from VERB code runs to quantify their relative importance to inner magnetospheric dynamics.…”

Section: Introductionmentioning

confidence: 99%

A Wave Model and Diffusion Coefficients for Plasmaspheric Hiss Parameterized by Plasmapause Location

2020

View full text Add to dashboard Cite

The scattering of electrons via plasmaspheric hiss whistler‐mode plasma waves has profound consequences for the dynamics of electrons in the inner terrestrial magnetosphere, including the radiation belts. Consequently, simulations of inner magnetospheric electron dynamics incorporate hiss wave models, though these models are often parameterized by quantities convenient to describe particle populations (e.g., L shell). However, recent studies have revealed that the spatial distribution of plasmaspheric hiss wave power is only weakly dependent on L shell. Instead, it is dictated by the density structure of the plasmasphere (including radial extent and azimuthal structure). In this work, we create a plasmaspheric hiss wave model, and corresponding particle diffusion coefficients, parameterized by plasmapause location instead of L shell, in order to quantify the importance of including plasmapause organization of hiss waves for inner magnetosphere models. Noticeable differences in electron scattering lifetimes are found when comparing L shell parameterized hiss and plasmapause‐parameterized hiss wave models on the timescales of days for 1 MeV electrons. Comparison of the lifetimes calculated from diffusion around the loss cone also show differences between L shell‐ and plasmapause‐parameterized hiss models. This implies that plasmapause parameterization of hiss waves may be important for modeling specific geomagnetic events.

show abstract

“…Circulation models cannot be applied for such small regions of space. Recent works on hiss within plumes (Hartley et al, 2019;Li et al, 2019;Nakamura et al, 2018;Shi et al, 2019;Teng et al, 2019;Zhang et al, 2018), although not the main focus of this paper, will be commented on in sections 4 and 5 of this paper in this light.…”

Section: Introductionmentioning

confidence: 99%

Low Frequency (f < 200 Hz) Polar Plasmaspheric Hiss: Coherent and Intense

et al. 2019

View full text Add to dashboard Cite

Low frequency (LF)~22 Hz to 200 Hz plasmaspheric hiss was studied using a year of Polar plasma wave data occurring during solar cycle minimum. The waves are found to be most intense in the noon and early dusk sectors. When only the most intense LF (ILF) hiss was examined, they are found to be substorm dependent and most prominent in the noon sector. The noon sector ILF waves were also determined to be independent of solar wind ram pressure. The ILF hiss intensity is independent of magnetic latitude. ILF hiss is found to be highly coherent in nature. ILF hiss propagates at all angles relative to the ambient magnetic field. Circular, elliptical, and linear/highly elliptically polarized hiss have been detected, with elliptical polarization the dominant characteristic. A case of linear polarized ILF hiss that occurred deep in the plasmasphere during geomagnetic quiet was noted. The waveforms and polarizations of ILF hiss are similar to those of intense high frequency hiss. We propose the hypothesis that~10-100 keV substorm injected electrons gradient drift to dayside minimum B pockets close to the magnetopause to generate LF chorus. The closeness of this chorus to low altitude entry points into the plasmasphere will minimize wave damping and allow intense noon-sector ILF hiss. The coherency of ILF hiss leads the authors to predict energetic electron precipitation into the mid latitude ionosphere and the electron slot formation during substorms. Several means of testing the above hypotheses are discussed.

show abstract

Quantification of Energetic Electron Precipitation Driven by Plume Whistler Mode Waves, Plasmaspheric Hiss, and Exohiss

Cited by 41 publications

References 59 publications

Earth's Van Allen Radiation Belts: From Discovery to the Van Allen Probes Era

Earth's Van Allen Radiation Belts: From Discovery to the Van Allen Probes Era

A Wave Model and Diffusion Coefficients for Plasmaspheric Hiss Parameterized by Plasmapause Location

Low Frequency (f < 200 Hz) Polar Plasmaspheric Hiss: Coherent and Intense

Contact Info

Product

Resources

About