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IMPTAM (1)

Inner Magnetosphere Particle Transport and Acceleration Model

Model Description

The IMPTAM (Ganushkina et al., 2005, 2012, 2014, 2015, 2023, 2024) distributions of ions (H+, O+, He+) and electrons in the drift approximation (first and second adiabatic invariants conserved) with arbitrary pitch angles from the plasma sheet (starting at 10 RE) to the inner L shell regions (2-3 RE) with energies reaching up to hundreds of keVs in time-dependent magnetic and electric fields. Relativistic effects for electrons are taken into account in the drift velocities. Liouville's theorem is used to gain information of the entire distribution function including loss process attenuation. For the obtained distribution we apply radial diffusion by solving the Fokker-Planck equation with Kp-dependent radial diffusion coefficients DLL for the magnetic field fluctuations. Details can be found in Ganushkina et al. (2012) for ions and Ganushkina et al. (2023) for electrons. 

IMPTAM is driven by (1) solar wind number density, (2) dynamic pressure, (3) velocity, (4) total strength and Y- and Z-components of IMF and (5) Dst and (6) Kp indices. In this version, inside IMPTAM, the set of models is (1) a dipole model for the internal magnetic field, (2) T96 model Tsyganenko (1995) for the external magnetic field, and (3) Boyle et al. (1997) polar cap potential mapped to the magnetosphere. We set the model boundary at 10 RE and use the kappa distribution function. Parameters of the kappa distribution function are the number density n and temperature T in the plasma sheet given by the empirical model derived from Geotail data for ions by Tsyganenko and Mukai (2023) and from THEMIS data by Dubyagin et al. (2016). 

IMPTAM is a flexible, module-based model so that it can use various representations for its main parts: particle transport, boundary conditions, background magnetic and electric fields, and loss processes.

Model Figure(s) :

Model Inputs Description

Solar wind number density, dynamic pressure, velocity, total strength and Y- and Z-components of IMF and Dst and Kp indices

Model Outputs Description

Ion (H+, O+, He+) and Electron fluxes in the energy range from 1 to 300 keV and pitch angle distributions everywhere in 3D inner magnetosphere at distances from 2 to 10 RE, with specific output at GEO, GTO and MEO orbits.

Model Caveats

Change Log

Version 1.1 includes all spieces.

Version 1.1 was deployed on the CCMC Continuous/Real-time Runs System on May 01, 2025.

Version 1.1 was deployed on the CCMC ROR System on May 19, 2025. 

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Curator: Chiu Wiegand | NASA Official: Dr. Masha Kuznetsova | Privacy and Security Notices | Accessibility | CCMC Data Collection Consent Agreement