As discussed in the Lecture, the Riemann Problem is the key pillar of Eulerian hydrodynamics and can not be
  solved fully analytically. In the lecture, we solved a special case of it. So, start with this picture
  
  taken from Simulation Techniques for Cosmological Simulations. Now, think about:
 Also, remember that we had the equation
  
  with
  
 
  
  to solve to get the solution for the pressure
  at the contact discontinuity (so pressure in sector 3 and 4). Think about:
  
You can start from the configuration of the code as obtained in T03 and collect some different particle distributions.
You can now write a program to set up a long slab (along the x-axis) which resembles your initial conditions.
Now you can run the simulation.
PERIODIC and
      NOGRAVITY again. Also, you have to indicate the non-cubic form
      of the simulation domain by setting LONG_X=100,
      LONG_Y=1 and LONG_Z=1
      in the Config.sh file before compiling.
    DesNumNgb,
      TimeMax,
      InitCondFile,
      BoxSize and
      SnapshotFileBase.
Goal of this tutorial is that you learn better how to create non-uniform initial conditions.
cp $HOME/Hydro/grid_10x10x10 .
      cp $HOME/Hydro/grid_12x12x12 .
    setup_slab.pro in IDL
    show_slab.pro in IDL
    
  
  ifort -g -traceback -check all -fpe0 -o slabsetup slabsetup.f90glass.txt, which is a text version of the glass file
        with coordinates in the range of 0 . . . 1)
      ./slabsetup
      gnuplot grid.plt (to check that the particle positions are set up correctly)
      LONG_X=20, LONG_Y=1, and LONG_Z=1
          (and PERIODIC and NOGRAVITY)
      slab.ic as the initial conditions file
          and output as the snapshot file base in the parameter file,
          and BoxSize 1
      ifort -g -traceback -check all -fpe0 -o readsnap readsnap.f90
      ./readsnap output_000 >output_000.txt
      ./readsnap output_010 >output_010.txt
      ./readsnap output_020 >output_020.txt
      gnuplot pressure.plt
      gv pressure.ps