The master script xsb3 computes ambient solar wind with a streamer belt (SB).
Boundary values of the solar wind velocity, density, temperature, and magnetic field strength (from left to right) at the boundary (at 0.1 AU):
[Image produced by plot_bnd.pro]
Distribution of the radial solar wind velocity on three slices passing trough the observing point “P03” (at 1 AU) and evolution at this point:
[Image produced by plot_tim3.pro]
Evolution of the solar wind radial velocity, number density, temperature, and magnetic field strength (from top to bottom) at the observing point “P03”:
[Image produced by plot_evo5o1.pro]
Execution of the master script xsb3 with default parameters produces results in the following sub-directories:
code.ra2low1.16-mcp1um1cd-1 with executables (ana3d3bc, enlil, out2evo)
case.ra2low1.b30d030d120t12t03v60v30-s30t40w0 with grid parameters (grd.nc) and boundary conditions (bnd.nc)
run.ra2low1.b30d030d120t12t03v60v30-s30t40w0.16-mcp1um1cd-1.g53t03b02 with values at time levels (tim.<rec>.nc) and evolution at observers (evo.<namobs>.nc and evo/evo.<namobs>.dat)
Numerical results evo/evo_p03.dat should be the same as the archived results doc/evo_p03.dat Values correspond to the evolution plot shown above.
The master script xsb3 can be copied and edited for different parameters of the ambient wind, coronal hole(s), and numerical model.
Alternatively, these parameters can be passed to the master script as arguments when it is executed. These modifications can be collected into a parametric script which executes the master script, under different conditions, as individual commands. Each run produces results into the “code”, “case”, and “run” directories named according to the used parameters.
Examples of parametric scripts:
Heliospheric results with tilt = 20 (top) and tilt = 60 (bottom)
[Images produced by plot_tim3e1.pro]
res = med (left) and res = high (right)
[Images produced by plot_evo5o1.pro]