CIMI

The Comprehensive Inner-Magnetosphere Ionosphere (CIMI) model is a bounce-averaged kinetic model of the ring current and radiation belts. This model calculates the temporal and spatial variation of the phase space density of ring current and radiation belt species: H+ and O+ in the energy range of 0.1 - 400 keV and electrons (e-) in the energy range of 1 - 4000 keV. The model considers particle drift in realistic, time-varying magnetic field, and self-consistent electric field that is solved taking into account current closure in the ionosphere. CIMI also considers charge exchange loss, energy and pitch-angle diffusion due to whistler mode chorus waves and plasmaspheric hiss. The simulation region is from the dayside magnetopause to the nightside boundary at 10-15 earth radii. The model is an initial-boundary-value problem, so initial distribution and boundary distribution as a function of time are required to run the model.

CIMI can be coupled with global MHD models. This type of code merging has been done with CIMI's predecessors: the CRCM (Comprehensive Ring Current Model) and RBE (Radiation Belt Environment) model [e.g., Glocer et al., 2011, 2013].

CIMI is thus a powerful tool for studying the dynamics of the ring current, radiation belts, and plasmasphere along with how they respond to solar wind input and their couplings with the ionosphere. Besides its various science applications, it also has great space weather potential.

Strengths: Combine the strengths of the Comprehensive Ring Current Model (CRCM) and the Radiation Belt Environment (RBE) model. Limitations: This version of CIMI uses empirical magnetic field models of T96 or T04. It does not consider the magnetic perturbation from the ring current and the transport due to MHD waves.

3D Magnetic Fields (Selection of Tsyganenko field models)

Ionospheric Electric Potentials at CIMI poleward boundary at 70.3° magnetic latitude (e.g., Weimer 2005)

Ionospheric quiet-time conductances (F10.7 solar irradiation index) and auroral conductances (Kp driven)

Solar wind speed, density and magnetic field, Dst, AE, AL index values to obtain plasma boundary conditions and drive the wave power model and magnetic field model

Equatorial H+, O+ and e- fluxes as functions of time, energy and pitch angle. Fluxes at off-equator can be obtained by mapping flux along a field line according to the equatorial pitch-angle distribution.

Plasmasphere density

Ionospheric potentials, Region 2 field aligned current and electron precipitation.

can be found in cimi.f90 (lines 122 -164) 122 ! February 1, 2019 123 ! - Add option for internal field: dipole or IGRF 124 ! September 27, 2019 125 ! - Add high order scheme to solve advection 126 ! June 11, 2020 127 ! - Set iplsh=4 for using geosyn data as boundary condition at rb 128 ! - Generalize varL to 1/(cos(xlati))^n 129 ! December 23, 2020 130 ! - add an option to use chorus diffusion coefficients and wave amplitude 131 ! from Qianli Ma at BU. 132 ! January 27, 2021 133 ! - The azimuth grid is changed from MLT to MLONG (geomagnetic longitude) 134 ! February 19, 2021 135 ! - xlati in 2D (xlati(i,j)) and guided by magnetic flux 136 ! April 9, 2021 137 ! - xlati in 2D (xlati(i,j)) and guided by flux tube volume per unit B flux 138 ! April 21, 2021 139 ! - add an option (icom) to estimate the O+/H+ and He+/H+ at the outer 140 ! boundary: 1=Young et al, 2,3=Pandya Bz, Psw 141 ! July 26, 2021 142 ! - xlati in 2D (xlati(i,j)) and guided by Euler potential alpha 143 ! February 9, 2022 144 ! - replace geopack_2005.f by geopack_2008.f 145 ! - use igrf routines in geopack_2008.f instead of those in IGRF12syn.f90 146 ! February 20, 2022 147 ! - use D_hiss_BU.dat instead of D_hiss_UCLA.dat. D_hiss_BU.dat covers 148 ! Fpe/Fce range from 1.2 to 30, while D_hiss_UCLA.dat covers only up to 20. 149 ! September 20, 2022 150 ! - Add an option (icP ge 3) to use Homayon Aryan's chorus wave model 151 ! https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2020JA028403 152 ! October 18, 2022 153 ! - Add an option (ihP=3) to use Homayon Aryan's hiss wave model 154 ! November 15, 2022 155 ! - Add an option (eplsh=3) to use Dubyagin's electron plasma sheet model 156 ! February 16, 2023 157 ! ~ Add fieldline-curvature scattering 158 ! April 24, 2023 159 ! - Add the calculation of corotation potential (potentc) and output in .pot 160 ! April 25, 2023 161 ! - Include ion precipitation in conductance calculation 162 ! April 25, 2024 163 ! - Weimer 2000 model is replaced by Weimer 2005 (w05sc_fok.f90) model 164 !************************