# Biblio

## Pages

**Authors:**Mithaiwala M J, and Horton W.

**Title:**

__Substorm injections produce sufficient electron energization to account for MeV flux enhancements following some storms__

**Abstract**: One of the main questions concerning radiation belt research is the origin of very high energy (>1 MeV) electrons following many space storms. Under the hypothesis that the plasma sheet electron population is the source of these electrons, which are convected to the outer radiation belt region during substorms, we estimate the flux of particles generated at geosynchronous orbit. We use the test particle method of following guiding center electrons as they drift in the electromagnetic fields during substorm dipolarization. The dipolarization pulse model electromagnetic fields are taken from the Li et al. (1998) substorm particle injection model. We find that a substorm dipolarization can produce enough electrons within geosynchronous orbit to account for the electrons seen following storms.. . .

**Date:**07/2005

**Publisher:**Journal of Geophysical Research

**DOI:**10.1029/2004JA010511

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/2004JA010511/abstract

*More Details***Authors:**Albert J M

**Title:**

__Evaluation of quasi-linear diffusion coefficients for whistler mode waves in a plasma with arbitrary density ratio__

**Abstract**: Techniques are presented for efficiently evaluating quasi-linear diffusion coefficients for whistler mode waves propagating according to the full cold plasma index of refraction. In particular, the density ratio ωpe/Ωe can be small, which favors energy diffusion. This generalizes an approach, previously used for high-density hiss and electromagnetic ion cyclotron waves, of identifying (and omitting) ranges of wavenormal angle θ that are incompatible with cyclotron resonant frequencies ω occurring between sharp cutoffs of the modeled wave frequency spectrum. This requires a detailed analysis of the maximum and minimum values of the refractive index as a function of ω and θ, as has previously been performed in the high-density approximation. Sample calculations show the effect of low-d. . .

**Date:**03/2005

**Publisher:**Journal of Geophysical Research

**DOI:**10.1029/2004JA010844

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/2004JA010844/abstract

*More Details***Authors:**Perry K L, Hudson M K, and Elkington S. R.

**Title:**

__Incorporating spectral characteristics of Pc5 waves into three-dimensional radiation belt modeling and the diffusion of relativistic electrons__

**Abstract**: The influence of ultralow frequency (ULF) waves in the Pc5 frequency range on radiation belt electrons in a compressed dipole magnetic field is examined. This is the first analysis in three dimensions utilizing model ULF wave electric and magnetic fields on the guiding center trajectories of relativistic electrons. A model is developed, describing magnetic and electric fields associated with poloidal mode Pc5 ULF waves. The frequency and L dependence of the ULF wave power are included in this model by incorporating published ground-based magnetometer data. It is demonstrated here that realistic spectral characteristics play a significant role in the rate of diffusion of relativistic electrons via drift resonance with poloidal mode ULF waves. Radial diffusion rates including bounce motion s. . .

**Date:**03/2005

**Publisher:**Journal of Geophysical Research

**DOI:**10.1029/2004JA010760

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/2004JA010760/abstract

*More Details***Authors:**Baker D N, Kanekal S G, Li X, Monk S P, Goldstein J,

*et al.*

**Title:**

__An extreme distortion of the Van Allen belt arising from the ‘Hallowe’en’ solar storm in 2003__

**Abstract**: The Earth's radiation belts—also known as the Van Allen belts1—contain high-energy electrons trapped on magnetic field lines2, 3. The centre of the outer belt is usually 20,000–25,000 km from Earth. The region between the belts is normally devoid of particles2, 3, 4, and is accordingly favoured as a location for spacecraft operation because of the benign environment5. Here we report that the outer Van Allen belt was compressed dramatically by a solar storm known as the ‘Hallowe'en storm’ of 2003. From 1 to 10 November, the outer belt had its centre only ~10,000 km from Earth's equatorial surface, and the plasmasphere was similarly displaced inwards. The region between the belts became the location of high particle radiation intensity. This remarkable deformation of the entire. . .

**Date:**12/2004

**Publisher:**Nature

**Pages:**878 - 881

**DOI:**10.1038/nature03116

**Available at:**http://www.nature.com/nature/journal/v432/n7019/full/nature03116.html

*More Details***Authors:**Shprits Y Y, and Thorne R. M.

**Title:**

__Time dependent radial diffusion modeling of relativistic electrons with realistic loss rates__

**Abstract**: Model simulations are compared to the typically observed evolution of MeV electron fluxes during geomagnetic storms to investigate whether radial diffusion alone can account for the observed variability and to estimate the effect of electron lifetimes. We demonstrate that knowledge of lifetimes is crucial for understanding the radial structure of the storm-time radiation belts and their temporal evolution. Our model results suggest that outer zone lifetimes at 1 MeV are on the order of few days during quite-times and less than a day during storm-time conditions. Losses outside plasmasphere should be included in the modeling of electron fluxes since effective lifetimes are much shorter than that of plasmaspheric losses. Simulations with variable outer boundary conditions show that the deple. . .

**Date:**04/2004

**Publisher:**Geophysical Research Letters

**DOI:**10.1029/2004GL019591

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/2004GL019591/abstract

*More Details***Authors:**Green Janet C, and Kivelson M. G.

**Title:**

__Relativistic electrons in the outer radiation belt: Differentiating between acceleration mechanisms__

**Abstract**: Many theoretical models have been developed to explain the rapid acceleration to relativistic energies of electrons that form the Earth's radiation belts. However, after decades of research, none of these models has been unambiguously confirmed by comparison to observations. Proposed models can be separated into two types: internal and external source acceleration mechanisms. Internal source acceleration mechanisms accelerate electrons already present in the inner magnetosphere (L < 6.6), while external source acceleration mechanisms transport and accelerate a source population of electrons from the outer to the inner magnetosphere. In principle, the two types of acceleration mechanisms can be differentiated because they imply that different radial gradients of electron phase space density. . .

**Date:**03/2004

**Publisher:**Journal of Geophysical Research

**DOI:**10.1029/2003JA010153

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/2003JA010153/abstract

*More Details***Authors:**O’Brien T P, Looper M. D., and Blake J. B.

**Title:**

__Quantification of relativistic electron microburst losses during the GEM storms__

**Abstract**: Bursty precipitation of relativistic electrons has been implicated as a major loss process during magnetic storms. One type of precipitation, microbursts, appears to contain enough electrons to empty the prestorm outer radiation belt in approximately a day. During storms that result in high fluxes of trapped relativistic electrons, microbursts continue for several days into the recovery phase, when trapped fluxes are dramatically increasing. The present study shows that this apparent inconsistency is resolved by observations that the number of electrons lost through microbursts is 10–100 times larger during the main phase than during the recovery phase of several magnetic storms chosen by the Geospace Environment Modeling (GEM) program.

**Date:**02/2004

**Publisher:**Geophysical Research Letters

**DOI:**10.1029/2003GL018621

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/2003GL018621/abstract

*More Details***Authors:**O’Brien T P, Lorentzen K. R., Mann I. R., Meredith N. P., Blake J. B.,

*et al.*

**Title:**

__Energization of relativistic electrons in the presence of ULF power and MeV microbursts: Evidence for dual ULF and VLF acceleration__

**Abstract**: We examine signatures of two types of waves that may be involved in the acceleration of energetic electrons in Earth's outer radiation belts. We have compiled a database of ULF wave power from SAMNET and IMAGE ground magnetometer stations for 1987–2001. Long-duration, comprehensive, in situ VLF/ELF chorus wave observations are not available, so we infer chorus wave activity from low-altitude SAMPEX observations of MeV electron microbursts for 1996–2001 since microbursts are thought to be caused by interactions between chorus and trapped electrons. We compare the ULF and microburst observations to in situ trapped electrons observed by high-altitude satellites from 1989–2001. We find that electron acceleration at low L shells is closely associated with both ULF activity and MeV microbu. . .

**Date:**08/2003

**Publisher:**Journal of Geophysical Research

**DOI:**10.1029/2002JA009784

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/2002JA009784/abstract

*More Details***Authors:**Albert J M

**Title:**

__Evaluation of quasi-linear diffusion coefficients for EMIC waves in a multispecies plasma__

**Abstract**: Quasi-linear velocity-space diffusion coefficients due to L-mode electromagnetic ion cyclotron (EMIC) waves are considered in a multispecies plasma. It is shown, with slight approximations to exact cold plasma theory, that within EMIC pass bands the index of refraction is a monotonically increasing function of frequency. Analytical criteria are then derived which identify ranges of latitude, wavenormal angle, and resonance number consistent with resonance in a prescribed wave population. This leads to computational techniques which allow very efficient calculation of the diffusion coefficients, along the lines previously developed for whistler and ion cyclotron waves in an electron-proton plasma. The techniques are applied to radiation belt electrons at L = 4, for EMIC waves in the hydroge. . .

**Date:**06/2003

**Publisher:**Journal of Geophysical Research

**DOI:**10.1029/2002JA009792

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/2002JA009792/abstract

*More Details***Authors:**Meredith Nigel P, Cain Michelle, Horne Richard B., Thorne Richard M., Summers D.,

*et al.*

**Title:**

__Evidence for chorus-driven electron acceleration to relativistic energies from a survey of geomagnetically disturbed periods__

**Abstract**: We perform a survey of the plasma wave and particle data from the CRRES satellite during 26 geomagnetically disturbed periods to investigate the viability of a local stochastic electron acceleration mechanism to relativistic energies driven by Doppler-shifted cyclotron resonant interactions with whistler mode chorus. Relativistic electron flux enhancements associated with moderate or strong storms may be seen over the whole outer zone (3 < L < 7), typically peaking in the range 4 < L < 5, whereas those associated with weak storms and intervals of prolonged substorm activity lacking a magnetic storm signature (PSALMSS) are typically observed further out in the regions 4 < L < 7 and 4.5 < L < 7, respectively. The most significant relativistic electron flux enhancements are seen outside of th. . .

**Date:**06/2003

**Publisher:**Journal of Geophysical Research

**DOI:**10.1029/2002JA009764

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/2002JA009764/abstract

*More Details***Authors:**Meredith Nigel P

**Title:**

__Statistical analysis of relativistic electron energies for cyclotron resonance with EMIC waves observed on CRRES__

**Abstract**: Electromagnetic ion cyclotron (EMIC) waves which propagate at frequencies below the proton gyrofrequency can undergo cyclotron resonant interactions with relativistic electrons in the outer radiation belt and cause pitch-angle scattering and electron loss to the atmosphere. Typical storm-time wave amplitudes of 1–10 nT cause strong diffusion scattering which may lead to significant relativistic electron loss at energies above the minimum energy for resonance, Emin. A statistical analysis of over 800 EMIC wave events observed on the CRRES spacecraft is performed to establish whether scattering can occur at geophysically interesting energies (≤2 MeV). While Emin is well above 2 MeV for the majority of these events, it can fall below 2 MeV in localized regions of high plasma density and/o. . .

**Date:**06/2003

**Publisher:**Journal of Geophysical Research

**DOI:**10.1029/2002JA009700

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/2002JA009700/full

*More Details***Authors:**Horne R B

**Title:**

__Relativistic electron acceleration and precipitation during resonant interactions with whistler-mode chorus__

**Abstract**: 1] Resonant interactions with whistler-mode chorus waves provide an important process for electron loss and acceleration during storm times. We demonstrate that wave propagation significantly affects the electron scattering rates. We show that stormtime chorus waves outside the plasmapause can scatter equatorial electrons ≤60 keV into the loss cone and accelerate trapped electrons up to ∼ MeV energies at large pitch-angles. Using ray tracing to map the waves to higher latitudes, we show that the decrease in the ratio between the electron plasma and gyro frequencies, along with the normalized chorus frequency bandwidth, enable much higher energy electrons ∼1 MeV to be scattered into the loss cone. We suggest that off equatorial pitch-angle scattering by chorus waves is responsible for. . .

**Date:**05/2003

**Publisher:**Geophysical Research Letters

**DOI:**10.1029/2003GL016973

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/2003GL016973/full

*More Details***Authors:**Summers D.

**Title:**

__Relativistic electron pitch-angle scattering by electromagnetic ion cyclotron waves during geomagnetic storms__

**Abstract**: [1] During magnetic storms, relativistic electrons execute nearly circular orbits about the Earth and traverse a spatially confined zone within the duskside plasmapause where electromagnetic ion cyclotron (EMIC) waves are preferentially excited. We examine the mechanism of electron pitch-angle diffusion by gyroresonant interaction with EMIC waves as a cause of relativistic electron precipitation loss from the outer radiation belt. Detailed calculations are carried out of electron cyclotron resonant pitch-angle diffusion coefficients Dαα for EMIC waves in a multi-ion (H+, He+, O+) plasma. A simple functional form for Dαα is used, based on quasi-linear theory that is valid for parallel-propagating, small-amplitude electromagnetic waves of general spectral density. For typical observed EM. . .

**Date:**04/2003

**Publisher:**Journal of Geophysical Research

**DOI:**10.1029/2002JA009489

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/2002JA009489/full

*More Details***Authors:**Miyoshi Yoshizumi

**Title:**

__Rebuilding process of the outer radiation belt during the 3 November 1993 magnetic storm: NOAA and Exos-D observations__

**Abstract**: Using the data from the NOAA and Exos-D satellites during the 3 November 1993 magnetic storm, the dynamic behavior of electrons with energies from a few tens of kiloelectronvolts to a few and its relation to plasma waves were examined. After the late main phase, relativistic electron flux started to recover from the heart of the outer radiation belt, where the cold plasma density was extremely low, and intense whistler mode chorus emissions were detected. The phase space density showed a peak in the outer belt, and the peak increased gradually. The simulation of the inward radial diffusion process could not reproduce the observed energy spectrum and phase space density variation. On the other hand, the simulated energy diffusion due to the gyroresonant electron-whistler mode wave interacti. . .

**Date:**03/2003

**Publisher:**Journal of Geophysical Research

**Pages:**SMP 3-1–SMP 3-15

**DOI:**10.1029/2001JA007542

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/2001JA007542/abstract

*More Details***Authors:**Elkington Scot R

**Title:**

__Resonant acceleration and diffusion of outer zone electrons in an asymmetric geomagnetic field__

**Abstract**: [1] The outer zone radiation belt consists of energetic electrons drifting in closed orbits encircling the Earth between ∼3 and 7 RE. Electron fluxes in the outer belt show a strong correlation with solar and magnetospheric activity, generally increasing during geomagnetic storms with associated high solar wind speeds, and increasing in the presence of magnetospheric ULF waves in the Pc-5 frequency range. In this paper, we examine the influence of Pc-5 ULF waves on energetic electrons drifting in an asymmetric, compressed dipole and find that such particles may be efficiently accelerated through a drift-resonant interaction with the waves. We find that the efficiency of this acceleration increases with increasing magnetospheric distortion (such as may be attributed to increased solar win. . .

**Date:**03/2003

**Publisher:**Journal of Geophysical Research

**DOI:**10.1029/2001JA009202

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/2001JA009202/full

*More Details***Authors:**Millan R M

**Title:**

__X-ray observations of MeV electron precipitation with a balloon-borne germanium spectrometer__

**Abstract**: The high-resolution germanium detector aboard the MAXIS (MeV Auroral X-ray Imaging and Spectroscopy) balloon payload detected nine X-ray bursts with significant flux extending above 0.5 MeV during an 18 day flight over Antarctica. These minutes-to-hours-long events are characterized by an extremely flat spectrum (∼E−2) similar to the first MeV event discovered in 1996, indicating that the bulk of parent precipitating electrons is at relativistic energies. The MeV bursts were detected between magnetic latitudes 58°–68° (L-values of 3.8–6.7) but only in the late afternoon/dusk sectors (14:30–00:00 MLT), suggesting scattering by EMIC (electromagnetic ion cyclotron) waves as a precipitation mechanism. We estimate the average flux of precipitating E ≥ 0.5 MeV electrons to be ∼36. . .

**Date:**12/2002

**Publisher:**Geophysical Research Letters

**DOI:**10.1029/2002GL015922

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/2002GL015922/full

*More Details***Authors:**ELKINGTON S, Hudson M K, Wiltberger M J, and Lyon J G

**Title:**

__MHD/particle simulations of radiation belt dynamics__

**Abstract**: Particle fluxes in the outer radiation belts can show substantial variation in time, over scales ranging from a few minutes, such as during the sudden commencement phase of geomagnetic storms, to the years-long variations associated with the progression of the solar cycle. As the energetic particles comprising these belts can pose a hazard to human activity in space, considerable effort has gone into understanding both the source of these particles and the physics governing their dynamical behavior. Computationally tracking individual test particles in a model magnetosphere represents a very direct, physically-based approach to modeling storm-time radiation belt dynamics. Using global magnetohydrodynamic models of the Earth–Sun system coupled with test particle simulations of the radiati. . .

**Date:**04/2002

**Publisher:**Journal of Atmospheric and Solar-Terrestrial Physics

**Pages:**607 - 615

**DOI:**10.1016/S1364-6826(02)00018-4

**Available at:**http://www.sciencedirect.com/science/article/pii/S1364682602000184

*More Details***Authors:**Ingraham J C, Cayton T E, Belian R D, Christensen R A, Friedel R H W,

*et al.*

**Title:**

__Substorm injection of relativistic electrons to geosynchronous orbit during the great magnetic storm of March 24, 1991__

**Abstract**: The great March 1991 magnetic storm and the immediately preceding solar energetic particle event (SEP) were among the largest observed during the past solar cycle, and have been the object of intense study. We investigate here, using data from eight satellites, the very large delayed buildup of relativistic electron flux in the outer zone during a 1.5-day period beginning 2 days after onset of the main phase of this storm. A notable feature of the March storm is the intense substorm activity throughout the period of the relativistic flux buildup, and the good correlation between some temporal features of the lower-energy substorm-injected electron flux and the relativistic electron flux at geosynchronous orbit. Velocity dispersion analysis of these fluxes between geosynchronous satellites . . .

**Date:**11/2001

**Publisher:**Journal of Geophysical Research

**Pages:**25759 - 25776

**DOI:**10.1029/2000JA000458

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/2000JA000458/full

*More Details***Authors:**Desorgher L, ühler P, Zehnder A, and ückiger E O

**Title:**

__Simulation of the outer radiation belt electron flux decrease during the March 26, 1995, magnetic storm__

**Abstract**: In this paper we study the variation of the relativistic electron fluxes in the Earth's outer radiation belt during the March 26, 1995, magnetic storm. Using observations by the radiation environment monitor (REM) on board the space technology research vehicle (STRV-Ib), we discuss the flux decrease and possible loss of relativistic electrons during the storm main phase. In order to explain the observations we have performed fully adiabatic and guiding center simulations for relativistic equatorial electrons in the nonstationary Tsygarienko96 magnetospheric magnetic field model. In our simulations the drift of electrons through the magnetopause was considered as a loss process. We present our model results and discuss their dependence on the magnetospheric magnetic and electric field model. . .

**Date:**09/2000

**Publisher:**Journal of Geophysical Research

**Pages:**21211

**DOI:**10.1029/2000JA900060

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/2000JA900060/full

*More Details***Authors:**Meredith Nigel P, Horne Richard B, Johnstone Alan D, and Anderson Roger R

**Title:**

__The temporal evolution of electron distributions and associated wave activity following substorm injections in the inner magnetosphere__

**Abstract**: The temporal evolution of electron distributions and associated wave activity following substorm injections in the inner magnetosphere are investigated using data from the CRRES satellite. Equatorial electron distributions and concomitant wave spectra outside the plasmapause on the nightside of the Earth are studied as a function of time since injection determined from the auroral-electrojet index (AE). The electron cyclotron harmonic (ECH) wave amplitudes are shown to be very sensitive to small modeling errors in the location of the magnetic equator. They are best understood at the ECH equator, defined by the local maximum in the ECH wave activity in the vicinity of the nominal magnetic equator, suggesting that the ECH equator is a better measure of the location of the true equator. Stron. . .

**Date:**06/2000

**Publisher:**Journal of Geophysical Research

**Pages:**12907

**DOI:**10.1029/2000JA900010

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/2000JA900010/full

*More Details***Authors:**Brautigam D H, and Albert J M

**Title:**

__Radial diffusion analysis of outer radiation belt electrons during the October 9, 1990, magnetic storm__

**Abstract**: The response of outer radiation belt relativistic electrons to the October 9, 1990, magnetic storm is analyzed in detail using a radial diffusion model and data from the Combined Release and Radiation Effects Satellite (CRRES) and the Los Alamos National Laboratory (LANL) geosynchronous satellite 1989-046. Electron measurements are expressed in terms of phase space density as a function of the three adiabatic invariants determined from CRRES magnetic field data and the Tsyganenko 1989 Kp-dependent magnetic field model. The radial diffusion model is implemented with a time-dependent radial diffusion coefficient parameterized by Kp, and a time-dependent outer boundary condition scaled by geosynchronous electron data. The results show that radial diffusion propagates outer boundary variations. . .

**Date:**01/2000

**Publisher:**Journal of Geophysical Research

**Pages:**291

**DOI:**10.1029/1999JA900344

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/1999JA900344/full

*More Details***Authors:**Elkington Scot R, Hudson M K, and Chan Anthony A

**Title:**

__Acceleration of relativistic electrons via drift-resonant interaction with toroidal-mode Pc-5 ULF oscillations__

**Abstract**: There has been increasing evidence that Pc-5 ULF oscillations play a fundamental role in the dynamics of outer zone electrons. In this work we examine the adiabatic response of electrons to toroidal-mode Pc-5 field line resonances using a simplified magnetic field model. We find that electrons can be adiabatically accelerated through a drift-resonant interaction with the waves, and present expressions describing the resonance condition and half-width for resonant interaction. The presence of magnetospheric convection electric fields is seen to increase the rate of resonant energization, and allow bulk acceleration of radiation belt electrons. Conditions leading to the greatest rate of acceleration in the proposed mechanism, a nonaxisymmetric magnetic field, superimposed toroidal oscillatio. . .

**Date:**11/1999

**Publisher:**Geophysical Research Letters

**Pages:**3273

**DOI:**10.1029/1999GL003659

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/1999GL003659/full

*More Details***Authors:**Burch L, Carovillano L, Antiochos K, Hudson M K, Elkington S R,

*et al.*

**Title:**

__Simulation of Radiation Belt Dynamics Driven by Solar Wind Variations__

**Abstract**: The rapid rise of relativistic electron fluxes inside geosynchronous orbit during the January 10-11, 1997, CME-driven magnetic cloud event has been simulated using a relativistic guiding center test particle code driven by out-put from a 3D global MHD simulation of the event. A comparison can be made of this event class, characterized by a moderate solar wind speed (< 600 km/s), and those commonly observed at the last solar maximum with a higher solar wind speed and shock accelerated solar energetic proton component. Relativistic electron flux increase occurred over several hours for the January event, during a period of prolonged southward IMF Bz more rapidly than the 1-2 day delay typical of flux increases driven by solar wind high speed stream interactions. Simulations of th. . .

**Date:**

**Publisher:**American Geophysical Union

**Pages:**171 - 182

**DOI:**10.1029/GM10910.1029/GM109p0171

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/GM109p0171/summary

*More Details***Authors:**Summers D., Thorne Richard M, and Xiao Fuliang

**Title:**

__Relativistic theory of wave-particle resonant diffusion with application to electron acceleration in the magnetosphere__

**Abstract**: Resonant diffusion curves for electron cyclotron resonance with field-aligned electromagnetic R mode and L mode electromagnetic ion cyclotron (EMIC) waves are constructed using a fully relativistic treatment. Analytical solutions are derived for the case of a single-ion plasma, and a numerical scheme is developed for the more realistic case of a multi-ion plasma. Diffusion curves are presented, for plasma parameters representative of the Earth's magnetosphere at locations both inside and outside the plasmapause. The results obtained indicate minimal electron energy change along the diffusion curves for resonant interaction with L mode waves. Intense storm time EMIC waves are therefore ineffective for electron stochastic acceleration, although these waves could induce rapid pitch angle scat. . .

**Date:**09/1998

**Publisher:**Journal of Geophysical Research

**Pages:**20487 - 20500

**DOI:**10.1029/98JA01740

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/98JA01740/abstract

*More Details***Authors:**Birn J, Thomsen M F, Borovsky J E, Reeves G D, McComas D J,

*et al.*

**Title:**

__Substorm electron injections: Geosynchronous observations and test particle simulations__

**Abstract**: We investigate electron acceleration and the flux increases associated with energetic electron injections on the basis of geosynchronous observations and test-electron orbits in the dynamic fields of a three-dimensional MHD simulation of neutral line formation and dipolarization in the magnetotail. This complements an earlier investigation of test protons [Birn et al., 1997b]. In the present paper we consider equatorial orbits only, using the gyrocenter drift approximation. It turns out that this approximation is valid for electrons prior to and during the flux rises observed in the near tail region of the model at all energies considered (∼ 100 eV to 1 MeV). The test particle model reproduces major observed characteristics: a fast flux rise, comparable to that of the ions, and the exist. . .

**Date:**05/1998

**Publisher:**Journal of Geophysical Research

**Pages:**9235 - 9248

**DOI:**10.1029/97JA02635

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/97JA02635/abstract

*More Details***Authors:**Abel Bob, and Thorne Richard M

**Title:**

__Electron scattering loss in Earth’s inner magnetosphere 1. Dominant physical processes__

**Abstract**: Pitch angle diffusion rates due to Coulomb collisions and resonant interactions with plasmaspheric hiss, lightning-induced whistlers and anthropogenic VLF transmissions are computed for inner magnetospheric electrons. The bounce-averaged, quasi-linear pitch angle diffusion coefficients are input into a pure pitch angle diffusion equation to obtain L and energy dependent equilibrium distribution functions and precipitation lifetimes. The relative effects of each scattering mechanism are considered as a function of electron energy and L shell. Model calculations accurately describe the enhanced loss rates in the slot region, as well as reduced scattering in the heavily populated inner radiation belt. Predicted electron distribution function calculations in the slot region display a character. . .

**Date:**02/1998

**Publisher:**Journal of Geophysical Research

**Pages:**2385 - 2396

**DOI:**10.1029/97JA02919

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/97JA02919/full

*More Details***Authors:**Li Xinlin, Baker D N, Temerin M, Cayton T E, Reeves E G D,

*et al.*

**Title:**

__Multisatellite observations of the outer zone electron variation during the November 3–4, 1993, magnetic storm__

**Abstract**: The disappearance and reappearance of outer zone energetic electrons during the November 3–4, 1993, magnetic storm is examined utilizing data from the Solar, Anomalous, and Magnetospheric Particle Explorer (SAMPEX), the Global Positioning System (GPS) series, and the Los Alamos National Laboratory (LANL) sensors onboard geosynchronous satellites. The relativistic electron flux drops during the main phase of the magnetic storm in association with the large negative interplanetary Bz and rapid solar wind pressure increase late on November 3. Outer zone electrons with E > 3 MeV measured by SAMPEX disappear for over 12 hours at the beginning of November 4. This represents a 3 orders of magnitude decrease down to the cosmic ray background of the detector. GPS and LANL sensors show similar eff. . .

**Date:**01/1997

**Publisher:**Journal of Geophysical Research

**Pages:**14123 - 14140

**DOI:**10.1029/97JA01101

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/97JA01101/abstract

*More Details***Authors:**Wygant J, Mozer F, Temerin M, Blake J, Maynard N,

*et al.*

**Title:**

__Large amplitude electric and magnetic field signatures in the inner magnetosphere during injection of 15 MeV electron drift echoes__

**Abstract**: Electric and magnetic fields were measured by the CRRES spacecraft at an L-value of 2.2 to 2.6 near 0300 magnetic local time during a strong storm sudden commencement (SSC) on March 24, 1991. The electric field signature at the spacecraft at the time of the SSC was characterized by a large amplitude oscillation (80 mV/m peak to peak) with a period corresponding to the 150 second drift echo period of the simultaneously observed 15 MeV electrons. Considerations of previous statistical studies of the magnitude of SSC electric and magnetic fields versus local time and analysis of the energization and cross-L transport of the particles imply the existence of 200 to 300 mV/m electric fields over much of the dayside magnetosphere. These observations also suggest that the 15 MeV drift echo electro. . .

**Date:**08/1994

**Publisher:**Geophysical Research Letters

**Pages:**1739–1742

**DOI:**10.1029/94GL00375

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/94GL00375/abstract

*More Details***Authors:**Li Xinlin, Roth I, Temerin M, Wygant J R, Hudson M K,

*et al.*

**Title:**

__Simulation of the prompt energization and transport of radiation belt particles during the March 24, 1991 SSC__

**Abstract**: We model the rapid (∼ 1 min) formation of a new electron radiation belt at L ≃ 2.5 that resulted from the Storm Sudden Commencement (SSC) of March 24, 1991 as observed by the CRRES satellite. Guided by the observed electric and magnetic fields, we represent the time-dependent magnetospheric electric field during the SSC by an asymmetric bipolar pulse that is associated with the compression and relaxation of the Earth's magnetic field. We follow the electrons using a relativistic guiding center code. The test-particle simulations show that electrons with energies of a few MeV at L > 6 were energized up to 40 MeV and transported to L ≃ 2.5 during a fraction of their drift period. The energization process conserves the first adiabatic invariant and is enhanced due to resonance of the el. . .

**Date:**11/1993

**Publisher:**Geophysical Research Letters

**Pages:**2423–2426

**DOI:**10.1029/93GL02701

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/93GL02701/abstract

*More Details***Authors:**Chiu Y T, Nightingale R W, and Rinaldi M A

**Title:**

__Simultaneous Radial and Pitch Angle Diffusion in the Outer Electron Radiation Belt__

**Abstract**: A solution of the bimodal (radial and pitch angle) diffusion equation for the radiation belts is developed with special regard for the requirements of satellite radiation belt data analysis. In this paper, we use this solution to test the bimodal theory of outer electron belt diffusion by confronting it with satellite data. Satellite observations, usually over finite volumes of (L, t) space, are seldom sufficient in space-time duration to cover the relaxation to equilibrium of the entire radiation belt. Since time scales of continuous data coverage are often comparable to that of radiation belt disturbances, it is therefore inappropriate to apply impulsive semi-infinite time response solutions of diffusion theory to interpret data from a finite window of (L, t) space. Observational limitat. . .

**Date:**04/1988

**Publisher:**Journal of Geophysical Research

**Pages:**2619 - 2632

**DOI:**10.1029/JA093iA04p02619

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/JA093iA04p02619/abstract

*More Details***Authors:**West H I, Buck R M, and Davidson G T

**Title:**

__The Dynamics of Energetic Electrons in the Earth’s Outer Radiation Belt During 1968 as Observed by the Lawrence Livermore National Laboratory’s Spectrometer on Ogo 5__

**Abstract**: An account is given of measurements of electrons made by the LLNL magnetic electron spectrometer (60–3000 keV in seven differential energy channels) on the Ogo 5 satellite in the earth's outer-belt regions during 1968 and early 1969. The data were analyzed to identify those features dominated by pitch angle and radial diffusion; in doing so all aspects of phase space covered by the data were studied, including pitch angle distributions and spectral features, as well as decay rates. The pitch angle distributions are reported elsewhere. The spectra observed in the weeks after a storm at L ∼3–4.5 show the evolution of a peak at ∼1.5 MeV and pronounced minima at ∼0.5 MeV. The observed pitch angle diffusion lifetimes are identified as being the shortest decays observed and are found t. . .

**Date:**04/1981

**Publisher:**Journal of Geophysical Research

**Pages:**2111 - 2142

**DOI:**10.1029/JA086iA04p02111

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/JA086iA04p02111/abstract

*More Details***Authors:**Holzworth R H, and Mozer F S

**Title:**

__Direct Evaluation of the Radial Diffusion Coefficient near L = 6 Due to Electric Field Fluctuations__

**Abstract**: The radial diffusion coefficient for radiation belt particles near L=6 has been calculated from the measured electric field fluctuations. Simultaneous balloon flights in August 1974 from six auroral zone sites ranging 180° in magnetic longitude produced the electric field data. The large scale slowly varying ionospheric electric fields from these flights have been mapped to the equator during the quiet magnetic conditions of this campaign. These mapped equatorial electric fields were then Fourier transformed in space and time to produce power spectra of the first two terms of the global azimuthal electric field. From these power spectra the radial diffusion coefficient has been calculated.

**Date:**06/1979

**Publisher:**Journal of Geophysical Research

**Pages:**2559 - 2566

**DOI:**10.1029/JA084iA06p02559

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/JA084iA06p02559/abstract

*More Details***Authors:**Lanzerotti L J, and Morgan Caroline G

**Title:**

__ULF Geomagnetic Power near__

*L*= 4, 2. Temporal Variation of the Radial Diffusion Coefficient for Relativistic Electrons**Abstract**: Measurements at conjugate points on the ground near L = 4 of the power spectra of magnetic-field fluctuations in the frequency range 0.5 to 20 mHz are used as a means of estimating daily values for the relativistic-electron radial-diffusion coefficient DLL for two periods in December 1971 and January 1972. The values deduced for L−10 DLL show a strong variation with magnetic activity, as measured by the Fredricksburg magnetic index KFR. The radial-diffusion coefficient typically increases by a factor of ∼10 for a unit increase in KFR. When KFR ≲ 2, it is generally found that DLL ≲ 2 × 10−9 L10 day−1 for equatorially mirroring electrons having a first invariant M = 750 Mev/gauss; a value of DLL ∼4 × 10−7 L10 day−1 is deduced for one day on which the mean KFR was 4.5. The. . .

**Date:**08/1973

**Publisher:**Journal of Geophysical Research

**Pages:**4600 - 4610

**DOI:**10.1029/JA078i022p04600

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/JA078i022p04600/abstract

*More Details***Authors:**Lyons Lawrence R, and Thorne Richard Mansergh

**Title:**

__Equilibrium Structure of Radiation Belt Electrons__

**Abstract**: The detailed quiet time structure of energetic electrons in the earth's radiation belts is explained on the basis of a balance between pitch angle scattering loss and inward radial diffusion from an average outer zone source. Losses are attributed to a combination of classical Coulomb scattering at low L and whistler mode turbulent pitch angle diffusion throughout the outer plasmasphere. Radial diffusion is driven by substorm associated fluctuations of the magnetospheric convection electric field.

**Date:**05/1973

**Publisher:**Journal of Geophysical Research

**Pages:**2142 - 2149

**DOI:**10.1029/JA078i013p02142

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/JA078i013p02142/abstract

*More Details***Authors:**Lyons Lawrence R, and Thorne Richard Mansergh

**Title:**

__Parasitic Pitch Angle Diffusion of Radiation Belt Particles by Ion Cyclotron Waves__

**Abstract**: The resonant pitch angle scattering of protons and electrons by ion cyclotron turbulence is investigated. The analysis is analogous to that recently performed for electron interactions with whistler mode waves. The role played by the intense band of ion cyclotron waves, predicted to be generated just within the plasmapause during the decay of the magnetospheric ring current, is evaluated in detail. Loss rates resulting from parasitic interactions with this turbulence are determined for energetic protons and relativistic electrons.

**Date:**10/1972

**Publisher:**Journal of Geophysical Research

**Pages:**5608 - 5616

**DOI:**10.1029/JA077i028p05608

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/JA077i028p05608/abstract

*More Details***Authors:**Tomassian Albert D, Farley Thomas A, and Vampola Alfred L

**Title:**

__Inner-Zone Energetic-Electron Repopulation by Radial Diffusion__

**Abstract**: A quantitative study of the intrusion of natural electrons into the inner radiation zone during and after the geomagnetic storm of September 2, 1966, shows that the transport is consistent with a radial-diffusion mechanism in which the first two invariants are conserved. Except for the 3-day period of the storm main phase when data were missing, the radial-diffusion coefficient is D = 2.7 × 10−5 L7.9 μ−0.5 day−1 in the range 1.7 ≤ L ≤ 2.6 and 13.3 ≤ μ ≤ 27.4 Mev gauss−1. This value could be produced by variation of a large-scale electric field across the magnetosphere having an amplitude of 0.28 mv / m and a period of 1600 sec. Electric fields having approximately these characteristics have been inferred from previous observations of the motion of whistler ducts within t. . .

**Date:**07/1972

**Publisher:**Journal of Geophysical Research

**Pages:**3441 - 3454

**DOI:**10.1029/JA077i019p03441

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/JA077i019p03441/abstract

*More Details***Authors:**Lanzerotti L J, Maclennan C G, and Schulz Michael

**Title:**

__Radial Diffusion of Outer-Zone Electrons: An Empirical Approach to Third-Invariant Violation__

**Abstract**: The near-equatorial fluxes of outer-zone electrons (E>0.5 Mev and E>1.9 Mev) measured by an instrument on the satellite Explorer 15 following the geomagnetic storm of December 17–18, 1962, are used to determine the electron radial diffusion coefficients and electron lifetimes as functions of L for selected values of the conserved first invariant µ. For each value of µ, the diffusion coefficient is assumed to be time-independent and representable in the form D = DnLn. The diffusion coefficients and lifetimes are then simultaneously obtained by requiring that the L-dependent reciprocal electron lifetime, as determined from the Fokker-Planck equation, deviate minimally from a constant in time. Applied to the data, these few assumptions yield a value of D that is smaller by approximately a. . .

**Date:**10/1970

**Publisher:**Journal of Geophysical Research

**Pages:**5351 - 5371

**DOI:**10.1029/JA075i028p05351

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/JA075i028p05351/abstract

*More Details***Authors:**Farley Thomas A

**Title:**

__Radial Diffusion of Starfish Electrons__

**Abstract**: A study of the change in electron intensities in the Starfish electron belt from January 1, 1963, to November 3, 1965, indicates that radial diffusion, both inward and outward from L of 1.40, was a significant loss mechanism for these electrons during this period. For L values of 1.20 and below, the indicated steepening of the pitch-angle distributions during this period has been interpreted as the result of a radial diffusion source for each L shell concentrated near the geomagnetic equator. Since pitch-angle diffusion lifetimes are not well known for 1.20 < L < 1.65, a definitive radial diffusion coefficient cannot be computed from these data. A maximum reasonable diffusion coefficient (mean square displacement per unit time) computed for this range of L for this period has a minimum at . . .

**Date:**07/1969

**Publisher:**Journal of Geophysical Research

**Pages:**3591 - 3600

**DOI:**10.1029/JA074i014p03591

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/JA074i014p03591/abstract

*More Details***Authors:**Birmingham Thomas J

**Title:**

__Convection Electric Fields and the Diffusion of Trapped Magnetospheric Radiation__

**Abstract**: We explore here the possible importance of time-dependent convection electric fields as an agent for diffusing trapped magnetospheric radiation inward toward the earth. By using a formalism (Birmingham, Northrop, and Fälthammar, 1967) based on first principles, and by adopting a simple model for the magnetosphere and its electric field, we succeed in deriving a one-dimensional diffusion equation to describe statistically the loss-free motion of mirroring particles with arbitrary but conserved values of the first two adiabatic invariants M and J. Solution of this equation bears out the fact that reasonable electric field strengths, correlated in time for no longer than the azimuthal drift period of an average particle, move particles toward the earth at a rate at least an order of magnitud. . .

**Date:**05/1969

**Publisher:**Journal of Geophysical Research

**Pages:**2169 - 2181

**DOI:**10.1029/JA074i009p02169

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/JA074i009p02169/abstract

*More Details***Authors:**Schulz Michael, and Eviatar Aharon

**Title:**

__Diffusion of Equatorial Particles in the Outer Radiation Zone__

**Abstract**: Expansions and contractions of the permanently compressed magnetosphere lead to the diffusion of equatorially trapped particles across drift shells. A general technique for obtaining the electric fields induced by these expansions and contractions is described and applied to the Mead geomagnetic field model. The resulting electric drifts are calculated and are superimposed upon the gradient drift executed by a particle that conserves its first (μ) and second (J = 0) adiabatic invariants. The noon-midnight asymmetry of the unperturbed drift trajectory (resulting from gradient drift alone) is approximated by means of a simple model. In this model the angular drift frequency is found to be the geometric mean of a particle's angular drift velocities at noon and midnight. The radial diffusion . . .

**Date:**05/1969

**Publisher:**Journal of Geophysical Research

**Pages:**2182 - 2192

**DOI:**10.1029/JA074i009p02182

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/JA074i009p02182/abstract

*More Details***Authors:**Vernov S N, Gorchakov E V, Kuznetsov S N, Logachev Yu. I, Sosnovets E N,

*et al.*

**Title:**

__Particle fluxes in the outer geomagnetic field__

**Abstract**: The outer geomagnetic field comprises the outer radiation belt, consisting of electrons with energies of 104–107 ev, and the unstable radiation zone. The outer radiation belt is bounded on its inner side by a gap, which is at various times located at a distance of 2.2–3.5 RE and in which a considerable precipitation of electrons from radiation belts occurs, possibly owing to a high intensity of electromagnetic waves. The boundary separating the outer radiation belt from the unstable radiation zone is at λ ∼ 71° and ∼9 RE in the equatorial plane on the sunlit side, and at 7–8 RE in the equatorial plane on the nightside. Beyond this, the unstable radiation zone extends out to the magnetosphere boundary and up to λ ∼ 77° on the sunlit side, and out to 14–15 RE on the nightsi. . .

**Date:**02/1969

**Publisher:**Reviews of Geophysics

**Pages:**257-280

**DOI:**10.1029/RG007i001p00257

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/RG007i001p00257/abstract

*More Details***Authors:**Newkirk L L, and Walt M

**Title:**

__Radial Diffusion Coefficient for Electrons at 1.76 <__

*L*< 5**Abstract**: Radial diffusion by nonconservation of the third adiabatic invariant of particle motion is assumed in analyzing experiments in which electrons appeared to move across field lines. Time-dependent solutions of the Fokker-Planck diffusion equation are obtained numerically and fitted to the experimental results by adjusting the diffusion coefficient. Values deduced for the diffusion coefficient vary from 1.3 × 10−5 RE²/day at L = 1.76 to 0.10 RE²/day at L = 5. In the interval 2.6 < L < 5, the coefficient varies as L10±1. Assuming a constant electron source of arbitrary magnitude at L = 6 and the above diffusion coefficients, the equatorial equilibrium distribution is calculated for electrons with energies above 1.6 Mev. The calculation yields an outer belt of electrons whose radial distr. . .

**Date:**12/1968

**Publisher:**Journal of Geophysical Research

**Pages:**7231 - 7236

**DOI:**10.1029/JA073i023p07231

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/JA073i023p07231/abstract

*More Details***Authors:**Newkirk L L, and Walt M

**Title:**

__Radial Diffusion Coefficient for Electrons at Low__

*L*Values**Abstract**: An empirical evaluation of the diffusion coefficient for trapped electrons diffusing across low L shells is obtained by adjusting the coefficient to account for the observed radial profile and the long-term decay rate of the trapped electron flux. The diffusion mechanism is not identified, but it is assumed that the adiabatic invariants µ and J are conserved. The average value of the coefficient for electrons > 1.6 Mev energy is found to decrease monotonically from ∼4 × 10−6 RE²/day at L = 1.16 to ∼2 × 10−7 RE²/day at L = 1.20.

**Date:**02/1968

**Publisher:**Journal of Geophysical Research

**Pages:**1013 - 1017

**DOI:**10.1029/JA073i003p01013

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/JA073i003p01013/abstract

*More Details***Authors:**Kennel C F

**Title:**

__Velocity Space Diffusion from Weak Plasma Turbulence in a Magnetic Field__

**Abstract**: The quasi‐linear velocity space diffusion is considered for waves of any oscillation branch propagating at an arbitrary angle to a uniform magnetic field in a spatially uniform plasma. The space‐averaged distribution function is assumed to change slowly compared to a gyroperiod and characteristic times of the wave motion. Nonlinear mode coupling is neglected. An H‐like theorem shows that both resonant and nonresonant quasi‐linear diffusion force the particle distributions towards marginal stablity. Creation of the marginally stable state in the presence of a sufficiently broad wave spectrum in general involves diffusing particles to infinite energies, and so the marginally stable plateau is not accessible physically, except in special cases. Resonant particles with velocities much . . .

**Date:**12/1966

**Publisher:**Physics of Fluids

**Pages:**2377

**DOI:**10.1063/1.1761629

**Available at:**http://scitation.aip.org/content/aip/journal/pof1/9/12/10.1063/1.1761629

*More Details***Authors:**Kennel C, and Petschek H

**Title:**

__Limit on Stably Trapped Particle Fluxes__

**Abstract**: Whistler mode noise leads to electron pitch angle diffusion. Similarly, ion cyclotron noise couples to ions. This diffusion results in particle precipitation into the ionosphere and creates a pitch angle distributon of trapped particles that is unstable to further wave growth. Since excessive wave growth leads to rapid diffusion and particle loss, the requirement that the growth rate be limited to the rate at which wave energy is depleted by wave propagation permits an estimate of an upper limit to the trapped equatorial particle flux. Electron fluxes >40 kev and proton fluxes >120 kev observed on Explorers 14 and 12, respectively, obey this limit with occasional exceptions. Beyond L = 4, the fluxes are just below their limit, indicating that an unspecified acceleration source, sufficient . . .

**Date:**01/1966

**Publisher:**Journal Geophysical Research

**Pages:**1-28

**DOI:**10.1029/JZ071i001p00001

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/JZ071i001p00001/full

*More Details***Authors:**Falthammar C -G

**Title:**

__Effects of time-dependent electric fields on geomagnetically trapped radiation.__

**Abstract**: Large-scale electric potential fields in the magnetosphere are generally invoked in theories of the aurora. It is shown in the present article that irregular fluctuations of such fields cause a random radial motion of trapped energetic particles by violating the third adiabatic invariant. When the first and second invariants are conserved, any radial motion of the particles is associated with a corresponding energy change. Some particles move outward and others inward; but, if there is a source in the outer magnetosphere and a sink farther in, there will be a net inward transport and an associated net energy gain. This mechanism supplements that of particle transport by magnetic disturbances, which has already been discussed in the literature. The transport and acceleration of energetic pa. . .

**Date:**06/1965

**Publisher:**Journal of Geophysical Research

**Pages:**2503–2516

**DOI:**10.1029/JZ070i011p02503

**Available at:**http://onlinelibrary.wiley.com/doi/10.1029/JZ070i011p02503/full

*More Details*