Tail plasma sheet models derived from Geotail particle data

By N. Tsyganenko, T. Mukai. 2003

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Simulation of the outer radiation belt electrons near geosynchronous orbit including both radial diffusion and resonant interaction with Whistler‐mode chorus waves (2005, background): “…by a kappa distribution f = 1032[1+ E/(kE0)] k 1 (in MeV 3s 3) with k = 5 and a characteristic energy of E0 = 5 keV, typical of the plasmasheet [Tsyganenko and Mukai, 2003], and where a kappa distribution is chosen to represent the high energy tail observed in the plasmasheet [e.g., Christon…”
Interaction between direct penetration and disturbance dynamo electric fields in the storm‐time equatorial ionosphere (2005, methodology): “The RCM simulation of this event utilized a time-sequence of Tsyganenko et al. [2003] storm-time magnetic-field models, a plasma sheet model [Tsyganenko and Mukai, 2003] as the outer boundary condition, and a time-sequence of polar cap potential drop values [Boyle et al., 1997].”
Average thermodynamic and spectral properties of plasma in and around dipolarizing flux bundles (2015, background): “Plasma sheet temperature and density depend on solar wind and interplanetary magnetic field conditions [Tsyganenko and Mukai, 2003].”