HR: 0800h
AN: SM21A-0336    [Abstracts]
TI: Radial diffusion with outer boundary determined by geosynchronous measurements: Storm and post-storm intervals
AU: * Chu, F
EM: feifei.chu@dartmouth.edu
AF: Dartmouth College, Physics and Astronomy Dept., Hanover, 03755,
AU: Haines, P
EM: paul.haines@dartmouth.edu
AF: Dartmouth College, Physics and Astronomy Dept., Hanover, 03755,
AU: Hudson, M
EM: mary.hudson@dartmouth.edu
AF: Dartmouth College, Physics and Astronomy Dept., Hanover, 03755,
AU: Kress, B
EM: bkress@dartmouth.edu
AF: Dartmouth College, Physics and Astronomy Dept., Hanover, 03755,
AU: Freidel, R
EM: rfreidel@lanl.gov
AF: LANL, ISR-1: SPACE SCIENCE AND APPLICATIONS, Los Alamos, NM 87545,
AU: Kanekal, S
EM: kanekal@lasp.colorado.edu
AF: LASP, University of Colorado, 1234 Innovation Dr., Boulder, CO 80303,
AB: Work is underway by several groups to quantify diffusive radial transport of radiation belt electrons, including a model for pitch angle scattering losses to the atmosphere. The radial diffusion model conserves the first and second adiabatic invariants and breaks the third invariant. We have developed a radial diffusion code which uses the Crank Nicholson method with a variable outer boundary condition. For the radial diffusion coefficient, DLL, we have several choices, including the Brautigam and Albert (JGR, 2000) diffusion coefficient parameterized by Kp, which provides an ad hoc measure of the power level at ULF wave frequencies in the range of electron drift (mHz), breaking the third invariant. Other diffusion coefficient models are Kp-independent, fixed in time but explicitly dependent on the first invariant, or energy at a fixed L, such as calculated by Elkington et al. (JGR, 2003) and Perry et al. (JGR, 2006) based on ULF wave model fields. We analyzed three periods of electron flux and phase space density (PSD) enhancements inside of geosynchronous orbit: March 31 – May 31, 1991, and July 2004 and Nov 2004 storm intervals. The radial diffusion calculation is initialized with a computed phase space density profile for the 1991 interval using differential flux values from the CRRES High Energy Electron Fluxmeter instrument, covering 0.65 - 7.5 MeV. To calculate the initial phase space density, we convert Roederer L* to McIlwain's L- parameter using the ONERA-DESP program. A time averaged model developed by Vampola1 from the entire 14 month CRRES data set is applied to the July 2004 and Nov 2004 storms. The online CRESS data for specific orbits and the Vampola-model flux are both expressed in McIlwain L-shell, while conversion to L* conserves phase space density in a distorted non-dipolar magnetic field model. A Tsyganenko (T04) magnetic field model is used for conversion between L* and L. The outer boundary PSD is updated using LANL GEO satellite fluxes. After calculating the phase space density time evolution for the two storms and post-injection interval (March 31 – May 31, 1991), we compare results with SAMPEX measurements. A better match with SAMPEX measurements is obtained with a variable outer boundary, also with a Kp-dependent diffusion coefficient, and finally with an energy and L-dependent loss term (Summers et al., JGR, 2004), than with a time-independent diffusion coefficient and a simple Kp-parametrized loss rate and location of the plasmapause. Addition of a varying outer boundary which incorporates measured fluxes at geosynchronous orbit using L* has the biggest effect of the three parametrized variations studied. 1Vampola, A.L., 1996, The ESA Outer Zone Electron Model Update, Environment Modelling for Spaced-based Applications, ESA SP-392, ESTEC, Nordwijk, NL, pp. 151-158, W. Burke and T.-D. Guyenne, eds.
DE: 2716 Energetic particles: precipitating
DE: 2730 Magnetosphere: inner
DE: 2736 Magnetosphere/ionosphere interactions (2431)
SC: SPA-Magnetospheric Physics [SM]
MN: 2007 Fall Meeting