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Modeling Radiation Belt Radial Diffusion In Ulf Wave Fields: 2. Estimating Rates Of Radial Diffusion Using Combined Mhd And Particle Codes, Chia-Lin L. Huang, Harlan E. Spence, Mary K. Hudson, Scot R. Elkington
Modeling Radiation Belt Radial Diffusion In Ulf Wave Fields: 2. Estimating Rates Of Radial Diffusion Using Combined Mhd And Particle Codes, Chia-Lin L. Huang, Harlan E. Spence, Mary K. Hudson, Scot R. Elkington
Physics & Astronomy
[1] Quantifying radial transport of radiation belt electrons in ULF wave fields is essential for understanding the variability of the trapped relativistic electrons. To estimate the radial diffusion coefficients (DLL), we follow MeV electrons in realistic magnetospheric configurations and wave fields calculated from a global MHD code. We create idealized pressure-driven MHD simulations for controlled solar wind velocities (hereafter referred to as pressure-driven Vx simulations) with ULF waves that are comparable to GOES data under similar conditions, by driving the MHD code with synthetic pressure profiles that mimic the pressure variations of a particular solar wind velocity. The ULF wave …
Modeling Radiation Belt Radial Diffusion In Ulf Wave Fields: 1. Quantifying Ulf Wave Power At Geosynchronous Orbit In Observations And In Global Mhd Model, Chia-Lin L. Huang, Harlan E. Spence, Howard J. Singer, W. Jeffrey Hughes
Modeling Radiation Belt Radial Diffusion In Ulf Wave Fields: 1. Quantifying Ulf Wave Power At Geosynchronous Orbit In Observations And In Global Mhd Model, Chia-Lin L. Huang, Harlan E. Spence, Howard J. Singer, W. Jeffrey Hughes
Physics & Astronomy
[1] To provide critical ULF wave field information for radial diffusion studies in the radiation belts, we quantify ULF wave power (f = 0.5–8.3 mHz) in GOES observations and magnetic field predictions from a global magnetospheric model. A statistical study of 9 years of GOES data reveals the wave local time distribution and power at geosynchronous orbit in field-aligned coordinates as functions of wave frequency, solar wind conditions (Vx, ΔPd and IMF Bz) and geomagnetic activity levels (Kp, Dst and AE). ULF wave power grows monotonically with increasing solar wind Vx, dynamic pressure variations ΔPd and geomagnetic indices in a …