Journal of Geophysical Research - Space Physics, ISSN 0148-0227, 03/2009, Volume 114, Issue A3, pp. A03201 - n/a

In this study, we develop a new code which uses a hybrid finite difference (HFD) method to solve a 2‐D bounce‐averaged energy–pitch angle diffusion equation in...

Numerical modeling | Radiation belts | Wave/particle interactions | Magnetospheric Physics | Substorms | Ionosphere | Energetic particles | precipitating | diffusion equation | hybrid finite difference method | wave‐particle interaction | OCTOBER 9 | ACCELERATION | ION-CYCLOTRON | GEOMAGNETIC STORMS | RELATIVISTIC ELECTRONS | CHORUS | ASTRONOMY & ASTROPHYSICS | PLASMASPHERIC HISS | SOLAR-WIND | RESONANT DIFFUSION | PITCH-ANGLE

Numerical modeling | Radiation belts | Wave/particle interactions | Magnetospheric Physics | Substorms | Ionosphere | Energetic particles | precipitating | diffusion equation | hybrid finite difference method | wave‐particle interaction | OCTOBER 9 | ACCELERATION | ION-CYCLOTRON | GEOMAGNETIC STORMS | RELATIVISTIC ELECTRONS | CHORUS | ASTRONOMY & ASTROPHYSICS | PLASMASPHERIC HISS | SOLAR-WIND | RESONANT DIFFUSION | PITCH-ANGLE

Journal Article

Journal of Geophysical Research: Space Physics, ISSN 2169-9380, 04/2018, Volume 123, Issue 4, pp. 2884 - 2901

In the presence of drift‐shell splitting intrinsic to the International Geomagnetic Reference Field magnetic field model, pitch angle scattering from Coulomb...

IGRF | neoclassical transport across low L‐shells | Coulomb collisions | radial diffusion | Fokker‐Planck equation | neoclassical transport across low L-shells | Fokker-Planck equation | FIELDS | PITCH-ANGLE SCATTERING | TRANSPORT | PLASMA | MOTION | ASTRONOMY & ASTROPHYSICS | MAGNETIC DRIFT SHELLS | MODEL | ENERGETIC PARTICLES | MAGNETOSPHERE | GEOMAGNETICALLY TRAPPED PARTICLES | Diffusion rate | Detonation | Radiation | Energy loss | Evolution | Mathematical models | Numerical models | Diffusion | Ionosphere | Geomagnetism | Decay rate | Computer simulation | Spacecraft | Fluxes | Splitting | Satellites | Trapped electrons | Low altitude | Atmosphere | Decay | Pitch (inclination) | Drift | Upper atmosphere | Magnetic fields | Altitude | Earth orbits | Electrons | NUCLEAR DISARMAMENT, SAFEGUARDS, AND PHYSICAL PROTECTION | 70 PLASMA PHYSICS AND FUSION TECHNOLOGY | ASTRONOMY AND ASTROPHYSICS | neoclassical diffusion | artificial radiation belts

IGRF | neoclassical transport across low L‐shells | Coulomb collisions | radial diffusion | Fokker‐Planck equation | neoclassical transport across low L-shells | Fokker-Planck equation | FIELDS | PITCH-ANGLE SCATTERING | TRANSPORT | PLASMA | MOTION | ASTRONOMY & ASTROPHYSICS | MAGNETIC DRIFT SHELLS | MODEL | ENERGETIC PARTICLES | MAGNETOSPHERE | GEOMAGNETICALLY TRAPPED PARTICLES | Diffusion rate | Detonation | Radiation | Energy loss | Evolution | Mathematical models | Numerical models | Diffusion | Ionosphere | Geomagnetism | Decay rate | Computer simulation | Spacecraft | Fluxes | Splitting | Satellites | Trapped electrons | Low altitude | Atmosphere | Decay | Pitch (inclination) | Drift | Upper atmosphere | Magnetic fields | Altitude | Earth orbits | Electrons | NUCLEAR DISARMAMENT, SAFEGUARDS, AND PHYSICAL PROTECTION | 70 PLASMA PHYSICS AND FUSION TECHNOLOGY | ASTRONOMY AND ASTROPHYSICS | neoclassical diffusion | artificial radiation belts

Journal Article

The Astrophysical Journal, ISSN 0004-637X, 02/2008, Volume 673, Issue 2, pp. 942 - 953

We consider the propagation of cosmic rays in turbulent magnetic fields. We use the models of magnetohydrodynamic turbulence that were tested in numerical...

MHD | Turbulence | Acceleration of particles | Scattering | Cosmic rays | ISM: magnetic fields | PITCH-ANGLE SCATTERING | acceleration of particles | turbulence | ANISOTROPY | ACCELERATION | PERTURBATION-THEORY | TRANSPORT | ISM : magnetic fields | cosmic rays | scattering | SCALING RELATIONS | CHARGED-PARTICLES | ASTRONOMY & ASTROPHYSICS | SPECTRUM | INTERSTELLAR TURBULENCE | COMPRESSIBLE MAGNETOHYDRODYNAMIC TURBULENCE | Physics - Cosmology and Nongalactic Astrophysics | Physics - Earth and Planetary Astrophysics | Physics - Instrumentation and Methods for Astrophysics | Physics - High Energy Astrophysical Phenomena | Physics - Solar and Stellar Astrophysics | Physics - Astrophysics of Galaxies

MHD | Turbulence | Acceleration of particles | Scattering | Cosmic rays | ISM: magnetic fields | PITCH-ANGLE SCATTERING | acceleration of particles | turbulence | ANISOTROPY | ACCELERATION | PERTURBATION-THEORY | TRANSPORT | ISM : magnetic fields | cosmic rays | scattering | SCALING RELATIONS | CHARGED-PARTICLES | ASTRONOMY & ASTROPHYSICS | SPECTRUM | INTERSTELLAR TURBULENCE | COMPRESSIBLE MAGNETOHYDRODYNAMIC TURBULENCE | Physics - Cosmology and Nongalactic Astrophysics | Physics - Earth and Planetary Astrophysics | Physics - Instrumentation and Methods for Astrophysics | Physics - High Energy Astrophysical Phenomena | Physics - Solar and Stellar Astrophysics | Physics - Astrophysics of Galaxies

Journal Article

Journal of Geophysical Research: Space Physics, ISSN 0148-0227, 05/2010, Volume 115, Issue A5, p. n/a

Using our recently introduced hybrid finite difference method, we develop a three‐dimensional (3‐D) code to solve a fully bounce‐averaged pitch‐angle and...

3D numerical modeling | wave‐particle interaction | radiation belts | ACCELERATION | ION-CYCLOTRON | WAVES | GEOMAGNETIC STORMS | RELATIVISTIC ELECTRONS | ASTRONOMY & ASTROPHYSICS | SOLAR-WIND | RESONANT DIFFUSION | PITCH-ANGLE | WHISTLER-MODE CHORUS | SCATTERING | Atmospheric sciences | Magnetism

3D numerical modeling | wave‐particle interaction | radiation belts | ACCELERATION | ION-CYCLOTRON | WAVES | GEOMAGNETIC STORMS | RELATIVISTIC ELECTRONS | ASTRONOMY & ASTROPHYSICS | SOLAR-WIND | RESONANT DIFFUSION | PITCH-ANGLE | WHISTLER-MODE CHORUS | SCATTERING | Atmospheric sciences | Magnetism

Journal Article

Journal of Geophysical Research: Space Physics, ISSN 2169-9380, 05/2017, Volume 122, Issue 5, pp. 5339 - 5354

Quasi‐linear diffusion coefficients are considered for highly oblique whistler mode waves, which exhibit a singular “resonance cone” in cold plasma theory. The...

quasi‐linear diffusion | oblique waves | radiation belts | quasi-linear diffusion | PITCH-ANGLE | PLASMA | RADIATION | ASTRONOMY & ASTROPHYSICS | DIPOLE | Approximation | Refractive index | Magnetic resonance | Refractivity | Exact solutions | Plasmasphere | Waves | Whistlers | Diffusion equations | Whistler waves | Resonance | Mathematical models | Kinetics | Diffusion coefficient | Diffusion | Plasma temperature | Electric fields | Formulas (mathematics)

quasi‐linear diffusion | oblique waves | radiation belts | quasi-linear diffusion | PITCH-ANGLE | PLASMA | RADIATION | ASTRONOMY & ASTROPHYSICS | DIPOLE | Approximation | Refractive index | Magnetic resonance | Refractivity | Exact solutions | Plasmasphere | Waves | Whistlers | Diffusion equations | Whistler waves | Resonance | Mathematical models | Kinetics | Diffusion coefficient | Diffusion | Plasma temperature | Electric fields | Formulas (mathematics)

Journal Article

Journal of Geophysical Research: Space Physics, ISSN 2169-9380, 05/2016, Volume 121, Issue 5, pp. 4217 - 4231

The radial and local diffusion processes induced by various plasma waves govern the highly energetic electron dynamics in the Earth's radiation belts, causing...

radiation belt simulation | energy‐dependent diffusion | electron acceleration and loss | radial diffusion | energy-dependent diffusion | EMIC WAVES | ION-CYCLOTRON | PITCH-ANGLE | ACCELERATION | RESONANT SCATTERING | GEOMAGNETIC STORMS | CHORUS WAVE | QUASI-LINEAR DIFFUSION | RELATIVISTIC ELECTRONS | ASTRONOMY & ASTROPHYSICS | COEFFICIENTS | Earth | Plasma | Simulation | Diffusion | Chorus | Radiation | Geomagnetic storms | Magnetosphere | Energy bands | Energy | Radiation belts | Astronomical instruments | ULF waves | Evolution | Electron diffusion | Electron density | Plasma waves | Geomagnetism | Diffusion processes | Magnetospheres | Electron fluxes | Storms | Wave scattering | Outer radiation belt | Pitch (inclination) | Magnetic storms | Scattering | Pitch angle | Three dimensional | Heliospheric and Magnetospheric Physics | CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS | GEOSCIENCES

radiation belt simulation | energy‐dependent diffusion | electron acceleration and loss | radial diffusion | energy-dependent diffusion | EMIC WAVES | ION-CYCLOTRON | PITCH-ANGLE | ACCELERATION | RESONANT SCATTERING | GEOMAGNETIC STORMS | CHORUS WAVE | QUASI-LINEAR DIFFUSION | RELATIVISTIC ELECTRONS | ASTRONOMY & ASTROPHYSICS | COEFFICIENTS | Earth | Plasma | Simulation | Diffusion | Chorus | Radiation | Geomagnetic storms | Magnetosphere | Energy bands | Energy | Radiation belts | Astronomical instruments | ULF waves | Evolution | Electron diffusion | Electron density | Plasma waves | Geomagnetism | Diffusion processes | Magnetospheres | Electron fluxes | Storms | Wave scattering | Outer radiation belt | Pitch (inclination) | Magnetic storms | Scattering | Pitch angle | Three dimensional | Heliospheric and Magnetospheric Physics | CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS | GEOSCIENCES

Journal Article

Journal of Geophysical Research: Space Physics, ISSN 0148-0227, 03/2010, Volume 115, Issue A3, p. n/a

The evolution of relativistic electron fluxes in the radiation belts is described by the modified Fokker‐Plank equation in terms of the radial distance, energy...

mixed diffusion | radiation belts | modeling | SALAMMBO CODE | ACCELERATION | DENSITY | MAGNETIC STORM | RELATIVISTIC ELECTRONS | PLASMASPHERE | ASTRONOMY & ASTROPHYSICS | PITCH-ANGLE DIFFUSION | TURBULENCE | MODEL | MAGNETOSPHERE | Atmospheric sciences | Magnetism

mixed diffusion | radiation belts | modeling | SALAMMBO CODE | ACCELERATION | DENSITY | MAGNETIC STORM | RELATIVISTIC ELECTRONS | PLASMASPHERE | ASTRONOMY & ASTROPHYSICS | PITCH-ANGLE DIFFUSION | TURBULENCE | MODEL | MAGNETOSPHERE | Atmospheric sciences | Magnetism

Journal Article

Journal of Geophysical Research: Space Physics, ISSN 2169-9380, 06/2013, Volume 118, Issue 6, pp. 3096 - 3112

Quantifying the loss of relativistic electrons from the Earth's radiation belts requires to estimate the effects of many kinds of observed waves, ranging from...

fast magnetosonic waves | lifetimes | radiation belts | quasi‐linear Diffusion | quasi-linear Diffusion | PITCH-ANGLE DIFFUSION | MAGNETOSPHERE | ACCELERATION | EQUATORIAL NOISE | PLASMA | ASTRONOMY & ASTROPHYSICS | COEFFICIENTS | RADIATION BELT ELECTRONS | CLUSTER | PROPAGATION | WHISTLER WAVES | Diffusion | Magnetic fields | Geophysics | Electrons | Sciences of the Universe

fast magnetosonic waves | lifetimes | radiation belts | quasi‐linear Diffusion | quasi-linear Diffusion | PITCH-ANGLE DIFFUSION | MAGNETOSPHERE | ACCELERATION | EQUATORIAL NOISE | PLASMA | ASTRONOMY & ASTROPHYSICS | COEFFICIENTS | RADIATION BELT ELECTRONS | CLUSTER | PROPAGATION | WHISTLER WAVES | Diffusion | Magnetic fields | Geophysics | Electrons | Sciences of the Universe

Journal Article

Journal of Geophysical Research - Space Physics, ISSN 0148-0227, 11/2006, Volume 111, Issue A11, pp. A11214 - n/a

Loss mechanisms responsible for the sudden depletions of the outer electron radiation belt are examined based on observations and radial diffusion modeling,...

Numerical modeling | trapped | Radiation belts | Magnetospheric Physics | Magnetosphere | inner | Energetic particles | precipitating | radial diffusion | magnetopause loss | wave‐particle interactions | EMIC WAVES | RELATIVISTIC ELECTRON FLUX | PITCH-ANGLE SCATTERING | MODE CHORUS WAVES | GEOMAGNETIC STORMS | PRECIPITATION | BELT ELECTRONS | MAGNETIC STORM | ASTRONOMY & ASTROPHYSICS | GEOSYNCHRONOUS ORBIT | ION-CYCLOTRON WAVES

Numerical modeling | trapped | Radiation belts | Magnetospheric Physics | Magnetosphere | inner | Energetic particles | precipitating | radial diffusion | magnetopause loss | wave‐particle interactions | EMIC WAVES | RELATIVISTIC ELECTRON FLUX | PITCH-ANGLE SCATTERING | MODE CHORUS WAVES | GEOMAGNETIC STORMS | PRECIPITATION | BELT ELECTRONS | MAGNETIC STORM | ASTRONOMY & ASTROPHYSICS | GEOSYNCHRONOUS ORBIT | ION-CYCLOTRON WAVES

Journal Article

Journal of Geophysical Research: Space Physics, ISSN 0148-0227, 03/2010, Volume 115, Issue A3, p. n/a

Radiation belt electrons and chorus waves are an outstanding instance of the important role cyclotron resonant wave‐particle interactions play in the...

quasi‐linear | diffusion | coherent | ACCELERATION | PLASMA | VLF WAVES | CHORUS | ASTRONOMY & ASTROPHYSICS | PITCH-ANGLE DIFFUSION | RESONANT DIFFUSION | MAGNETIC-FIELD | RADIATION BELT ELECTRONS | MAGNETOSPHERE | WHISTLER WAVES | Space | Plasma physics | Magnetism | Atmospheric sciences

quasi‐linear | diffusion | coherent | ACCELERATION | PLASMA | VLF WAVES | CHORUS | ASTRONOMY & ASTROPHYSICS | PITCH-ANGLE DIFFUSION | RESONANT DIFFUSION | MAGNETIC-FIELD | RADIATION BELT ELECTRONS | MAGNETOSPHERE | WHISTLER WAVES | Space | Plasma physics | Magnetism | Atmospheric sciences

Journal Article

Journal of Geophysical Research: Space Physics, ISSN 0148-0227, 06/2012, Volume 117, Issue A6, p. n/a

The loss of relativistic electrons from the Earth's radiation belts can be described in terms of the quasi‐linear pitch angle diffusion by cyclotron‐resonant...

lifetime | radiation belts | chorus | quasi‐linear diffusion | GYROFREQUENCY VLF EMISSIONS | TRAPPED-PARTICLES | RESONANT INTERACTIONS | SOURCE REGION | ASTRONOMY & ASTROPHYSICS | SOLAR-WIND | PITCH-ANGLE DIFFUSION | WHISTLER-MODE WAVES | RADIATION BELT ELECTRONS | OUTER MAGNETOSPHERE | PROPAGATION | Space | Weather | Magnetism | Atmospheric sciences | Radiation

lifetime | radiation belts | chorus | quasi‐linear diffusion | GYROFREQUENCY VLF EMISSIONS | TRAPPED-PARTICLES | RESONANT INTERACTIONS | SOURCE REGION | ASTRONOMY & ASTROPHYSICS | SOLAR-WIND | PITCH-ANGLE DIFFUSION | WHISTLER-MODE WAVES | RADIATION BELT ELECTRONS | OUTER MAGNETOSPHERE | PROPAGATION | Space | Weather | Magnetism | Atmospheric sciences | Radiation

Journal Article

Journal of Geophysical Research: Space Physics, ISSN 2169-9380, 11/2019, Volume 124, Issue 11, pp. 8488 - 8506

In the outer radiation belt, the acceleration and loss of high‐energy electrons is largely controlled by wave‐particle interactions. Quasilinear diffusion...

parameterization | empirical | stochastic | magnetosphere | wave‐particle interactions | PITCH-ANGLE | wave-particle interactions | WHISTLER-MODE CHORUS | ACCELERATION | RESONANT SCATTERING | ELECTRON-RADIATION BELTS | ASTRONOMY & ASTROPHYSICS | WAVE ACTIVITY | FREQUENCY | STATISTICAL PROPERTIES | Plasma | Weather forecasting | Variability | Radiation | Parameterization | Density | Energy | Radiation belts | Temporal variability | Particle interactions | Statistical distributions | Electromagnetic waves | Mathematical models | Diffusion | Diffusion coefficient | Geomagnetic activity | Magnetic properties | In situ measurement | Geomagnetism | Composition | Natural variability | Computer simulation | Geophysics | Electromagnetic radiation | Magnetospheres | Physics | Geophysical methods | Field strength | Bins | Outer radiation belt | Pitch (inclination) | Magnetic fields | Acceleration | Electrons

parameterization | empirical | stochastic | magnetosphere | wave‐particle interactions | PITCH-ANGLE | wave-particle interactions | WHISTLER-MODE CHORUS | ACCELERATION | RESONANT SCATTERING | ELECTRON-RADIATION BELTS | ASTRONOMY & ASTROPHYSICS | WAVE ACTIVITY | FREQUENCY | STATISTICAL PROPERTIES | Plasma | Weather forecasting | Variability | Radiation | Parameterization | Density | Energy | Radiation belts | Temporal variability | Particle interactions | Statistical distributions | Electromagnetic waves | Mathematical models | Diffusion | Diffusion coefficient | Geomagnetic activity | Magnetic properties | In situ measurement | Geomagnetism | Composition | Natural variability | Computer simulation | Geophysics | Electromagnetic radiation | Magnetospheres | Physics | Geophysical methods | Field strength | Bins | Outer radiation belt | Pitch (inclination) | Magnetic fields | Acceleration | Electrons

Journal Article

Journal of Geophysical Research: Space Physics, ISSN 2169-9380, 10/2013, Volume 118, Issue 10, pp. 6197 - 6211

As a response to the Geospace Environment Modeling (GEM) “Global Radiation Belt Modeling Challenge,” a 3D diffusion model is used to simulate the radiation...

GEM challenge | Radiation belt electrons | DREAM3D | 3D diffusion model | PITCH-ANGLE SCATTERING | MAGNETIC STORMS | FIELD | ION-CYCLOTRON WAVES | ACCELERATION | INNER MAGNETOSPHERE | GEOMAGNETIC STORMS | RELATIVISTIC ELECTRONS | ASTRONOMY & ASTROPHYSICS | RESONANT DIFFUSION | CRRES OBSERVATIONS | Boundary conditions | Models | Kinetics | Diffusion | Radiation

GEM challenge | Radiation belt electrons | DREAM3D | 3D diffusion model | PITCH-ANGLE SCATTERING | MAGNETIC STORMS | FIELD | ION-CYCLOTRON WAVES | ACCELERATION | INNER MAGNETOSPHERE | GEOMAGNETIC STORMS | RELATIVISTIC ELECTRONS | ASTRONOMY & ASTROPHYSICS | RESONANT DIFFUSION | CRRES OBSERVATIONS | Boundary conditions | Models | Kinetics | Diffusion | Radiation

Journal Article