Van Allen Probes observations of prompt MeV radiation belt electron acceleration in nonlinear interactions with VLF chorus

Foster, J. C.; Erickson, P. J.; Omura, Yoshiharu; Baker, D. N.; Kletzing, C. A.; Claudepierre, S. G.

doi:10.1002/2016ja023429

Cited by 96 publications

(131 citation statements)

References 55 publications

(98 reference statements)

Supporting

Mentioning

121

Contrasting

Order By: Relevance

“…Other articles demonstrate the significance of pitchangle diffusion in velocities for electron flux increases (Summers et al, 1998;Horne et al, 2005;Demekhov et al, 2006;Foster et al, 2017]. Acceleration to energies of the order of 1 MeV occurs in RB with a maximum at L~4-7.…”

Section: Interaction Of Electrons With High-frequency Wavesmentioning

confidence: 98%

“…Along with the cyclotron resonance, we can expect a drift resonance with magnetospheric Pc5 pulsations or solar wind pulsations with a period of the order of several minutes. Acceleration of this type is mentioned, say, in [Elkington et al, 1999;Ukhorskiy et al, 2006]. The acceleration of electrons due to the radial electric drift or their shift to the region of a stronger magnetic field is faster and more efficient.…”

Section: Acceleration Processes Slow E×b Driftmentioning

confidence: 99%

See 1 more Smart Citation

Electron radiation belt dynamics during magnetic storms and in quiet time

Lazutin¹,

Дмитриев²,

Дмитриев

et al. 2018

Solar-Terrestrial Physics

View full text Add to dashboard Cite

Abstract. The paper discusses the outer electron belt dynamics, adiabatic and nonadiabatic mechanisms of increases and losses of energetic electrons.Under undisturbed conditions, the outer electron belt gradually empties: in the inner magnetosphere due to electron losses in the atmosphere and in the quasitrapping region due to losses at the magnetopause because drift shells of electrons are not closed there. The latter process does not occur in normal years due to the masking replenishment by freshly accelerated particles, but in years of extremely low activity it leads to a significant decrease in the electron population of the belt.During the magnetic storm main phase, the first reason for the decrease in the electron flux intensity is the adiabatic cooling associated with conservation of adiabatic invariants and complemented by injection of electrons into the atmosphere and their losses at the magnetopause. Electron flux increases involve E×B electron injection by the induction electric field of substorm activation and by the large-scale solar wind electric field, with pitch energy diffusion along with adiabatic heating in the recovery phase.The rate of electron flux recovery after a storm is determined by the ratio of nonadiabatic increases and losses; hence the electron flux represents a continuous series from low to very high values. The combination of these processes determines the individual character of radiation belt development during each magnetic storm and the behavior of the belt in the quiet time.

show abstract

Section: Interaction Of Electrons With High-frequency Wavesmentioning

confidence: 98%

Section: Acceleration Processes Slow E×b Driftmentioning

confidence: 99%

Electron radiation belt dynamics during magnetic storms and in quiet time

Lazutin¹,

Дмитриев²,

Дмитриев

et al. 2018

Solar-Terrestrial Physics

View full text Add to dashboard Cite

show abstract

“…The rapid increase in MeV electron fluxes associated with substorm injections suggests that nonlinear processes, with associated rapid interaction time scales, play a significant role Foster et al 2017) in the local acceleration process (Foster et al 2017). Wave-electron interactions during the generation of VLF rising tones are strongly non-linear, leading the formation of a highly coherent wave structure.…”

Section: Local Acceleration By Vlf Chorusmentioning

confidence: 99%

“…For phase trapped resonant electrons with near-relativistic initial energies, well-developed subpackets at and around 1/4 f ce result in strong (>100 keV) energy gain through nonlinear relativistic turning acceleration (RTA) (Omura et al 2007) for electrons with relativistic initial energies (Foster et al 2017). Electrons with initial energy 100s keV-3 MeV can be accelerated by 50 keV-200 keV in resonant interactions with a single VLF rising tone on a time scale of 10-100 msec (Foster et al 2017).…”

Section: Local Acceleration By Vlf Chorusmentioning

confidence: 99%

See 1 more Smart Citation

Space Weather Effects in the Earth’s Radiation Belts

et al. 2017

Self Cite

View full text Add to dashboard Cite

The first major scientific discovery of the Space Age was that the Earth is enshrouded in toroids, or belts, of very high-energy magnetically trapped charged particles. Early observations of the radiation environment clearly indicated that the Van Allen belts could be delineated into an inner zone dominated by high-energy protons and an outer zone dominated by high-energy electrons. The energy distribution, spatial extent and particle species makeup of the Van Allen belts has been subsequently explored by several space missions. Recent observations by the NASA dual-spacecraft Van Allen Probes mission have revealed many novel properties of the radiation belts, especially for electrons at highly relativistic and ultra-relativistic kinetic energies. In this review we summarize the space weather impacts of the radiation belts. We demonstrate that many remarkable features of energetic particle changes are driven by strong solar and solar wind forcings. Recent comprehensive data show broadly and in many ways how high energy particles are accelerated, transported, and lost in the magnetosphere due to interplanetary shock wave interactions, coronal mass ejection impacts, and high-speed solar wind streams. We also discuss how radiation belt particles are intimately tied to other parts of the geospace system through atmosphere, ionosphere, and plasmasphere coupling. The new data have in many ways rewritten the textbooks about the radiation belts as a key space weather threat to human technological systems.

show abstract

Radiation belt seed population and its association with the relativistic electron dynamics: A statistical study

Tang

Wang

et al. 2017

JGR Space Physics

Self Cite

View full text Add to dashboard Cite

Using the particle data measured by Van Allen Probe A from October 2012 to March 2016, we investigate in detail the radiation belt seed population and its association with the relativistic electron dynamics during 74 geomagnetic storms. The period of the storm recovery phase was limited to 72 h. The statistical study shows that geomagnetic storms and substorms play important roles in the radiation belt seed population (336 keV electrons) dynamics. Based on the flux changes of 1 MeV electrons before and after the storm peak, these storm events are divided into two groups of “large flux enhancement” and “small flux enhancement.” For large flux enhancement storm events, the correlation coefficients between the peak flux location of the seed population and those of relativistic electrons (592 keV, 1 MeV, 1.8 MeV, and 2.1 MeV) during the storm recovery phase decrease with electron kinetic energy, being 0.92, 0.68, 0.49, and 0.39, respectively. The correlation coefficients between the peak flux of the seed population and those of relativistic electrons are 0.92, 0.81, 0.75, and 0.73. For small flux enhancement storm events, the correlation coefficients between the peak flux location of the seed population and those of relativistic electrons are relatively smaller, while the peak flux of the seed population is well correlated with those of relativistic electrons (correlation coefficients >0.84). It is suggested that during geomagnetic storms there is a good correlation between the seed population and ≤1 MeV electrons and the seed population is important to the relativistic electron dynamics.

show abstract

Van Allen Probes observations of prompt MeV radiation belt electron acceleration in nonlinear interactions with VLF chorus

Cited by 96 publications

References 55 publications

Electron radiation belt dynamics during magnetic storms and in quiet time

Electron radiation belt dynamics during magnetic storms and in quiet time

Space Weather Effects in the Earth’s Radiation Belts

Radiation belt seed population and its association with the relativistic electron dynamics: A statistical study

Contact Info

Product

Resources

About