Examples

Basic 1D Usage

In Python, run:

from Mshpy import msh_param

Then you can run msh_param as follows:

msh_param('test', '2012-03-01T02:00', '2012-03-01T04:00', 'cluster4', mpoff=0, bsoff=0.08)

  • path: Output directory for the result file. If you are using a custom spacecraft trace file, refer to the ‘Usage’ section for detailed format requirements.

Note: The model magnetopause and bow shock positions may not perfectly match actual boundaries. Manual offset (mpoff, bsoff) may be needed based on satellite boundary crossing data.

To plot the result:

from Mshpy import Msh_sc_data
Msh_sc_data.main(['test', '2012-03-01T02:00', '2012-03-01T04:00', 'cluster4'])

3D Output Example

To generate 3D output:

from Mshpy import Msh_Nstep_3D
Msh_Nstep_3D.main(x, y, z, f_sw, fout)

  • x, y, z: 1D arrays (e.g., from numpy.linspace) defining the 3D spatial grid in GSE coordinates (Re).

  • f_sw: Input solar wind data file in the following format :

Bx By Bz Vx Vy Vz n Pd Ma Mm

Each column represents:

  • Bx, By, Bz: Interplanetary magnetic field components (nT, in GSE)

  • Vx, Vy, Vz: Solar wind velocity components (km/s, in GSE)

  • n: Proton number density (cm⁻³)

  • Pd: Dynamic pressure (nPa)

  • Ma: Alfvén Mach number

  • Mm: Magnetosonic Mach number

This format follows OMNIweb, for example:

2 -2 -5 -400 0 0 10 2 10 6

  • fout: Output netCDF file name to store the computed plasma and magnetic field quantities on the 3D grid.

This will create a netCDF file containing variables like Bx, By, Bz, n, T, Vx, Vy, Vz, along with coordinate axes x, y, z.