The master script xch3cone computes propagation of a heliospheric disturbance initiated by the Cone model in the ambient solar wind with a coronal hole (CH).
Boundary values of the solar wind velocity, density, temperature, and magnetic field strength (from left to right) at time when a hydrodynamic ejecta passes 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_tim3e1.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 xch3cone with default parameters produces results in the following sub-directories:
code.ra2low2.16-mcp1um1cd-1 with executables (ana3d3bc, enlil, out2evo)
case.ra2low2.b30d60t06v30-h45n0w0-d4t1v900r30p2 with grid parameters (grd.nc) and boundary conditions (bnd.nc)
run.ra2low2.b30d120t03v30-h30n0w0-g53x00-d4t1v900r30p2.16-mcp1um1cd-1.t03b02 with values at time levels (tim.<rec>.nc) and evolution at observers (evo.<namobs>.nc and evo/evo.<namobs>.dat)
Numerical results evo/evo1_p03.dat should be the same as doc/evo1_p03.dat.
The master script xch3cone can be copied and edited for computing with 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:
zch3cone-dist runs xch3cone with different positions of the CH:
hlon = -60
hlon = -30
hlon = 30
hlon = 60
[Images produced by plot_tim3e1.pro]