The Tsyganenko and Mukai Plasmasheet Model (TM2003) is an analytical models which parameterizes the 2-D
distribution (along and across the Earth’s magnetotail) of the central plasma sheet (CPS) ion temperature, density, and pressure, as functions of the incoming solar wind and interplanetary magnetic field (IMF) parameters, at distances between 10 and 50 RE. The model uses the Shue, et. al. magnetopause model to determine the dimensions of the central plasmasheet, and hence the limits of validity. This matlab implementation can operate on a grid of Geocentric Solar Magnetic coordinates.
XGSM - [Re] geocentric solar magnetic (GSM) X-axis points to Sun
YGSM - [Re] geocentric solar magnetic (GSM) X-hat x Y-hat = Z-hat
ZGSM - [Re] geocentric solar magnetic (GSM) projection of the Earth's magnetic dipole axis (positive North) on to the plane perpendicular to the X axis
Densw - [1/cm^3] solar wind proton density in cc^-1
Vsw - [km/s] solar wind speed
ByIMF - [GSM, nT] IMF By
BzIMF - [GSM, nT] IMF Bz
Plasmasheet_Density_per_cm3 - [protons/cm3] plasmasheet proton density
Plasmasheet_Pressure_nPa - [nPa] plasma sheet ion pressure
Plasmasheet_Temperature_keV - [keV] plasma sheet proton temperature
The Table 1 coefficients are taken from the fortran model provided by Tysgenenko, since there is a higher precision therein than in the paper.
The examples recreate Figures 9, 10, and 11 from the paper.
Tsyganenko, N. A.0, and T. Mukai, Tail plasma sheet models derived from Geotail particle data, J. Geophys. Res.0, 108(A3), 1136, doi:10.1029/2002JA009707, 2003.
Shue, J.-H., et al., Magnetopause location under extreme solar wind conditions, J. Geophys. Res., 103, 17, 691, 1998.
Meg Noah (2023). Tsyganenko and Mukai Plasmasheet Model (T, P, Density) (https://www.mathworks.com/matlabcentral/fileexchange/71957-tsyganenko-and-mukai-plasmasheet-model-t-p-density), MATLAB Central File Exchange. Retrieved .
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