The radiative cooling is described by the cooling function which is based on what kinds of interactions will occur depending on the composition of the gas and its current temperature. These are 1D radiative tests of the cooling added to the WOMBAT code.
These are 1D radiative cooling tests of steady state solutions for various shocks and cooling functions. These tests start by using the steady state solution for an adiabatic shock, solved numerically using a Runge-Kutta solver. This is then inputed as initial conditions into the Riemann solver which should evolve the shock into a steady state, non-adiabatic, shock by applying a shift in the velocity such that the shock is at rest in the rest frame of the Riemann solver. The upstream values of this shock are then used in the Runge-Kutta to solve for the steady state solution of this new shock (shown in black in the plots below). This should now give the same answer as the Riemann solver and so the steady state solution given by the Runge-Kutta is set as the initial conditions for the code. This final shock is then evolved over time to see if the code will keep the same steady state.
2D & 3D
The first set of 2D and 3D tests are the same as the 1D steady state tests but copied over into the other dimensions. We tested the lower Mach number with the shock front perpendicular to the x-axis, the y-axis and at axis rotated by 45 and 22.5 degrees.
The attached movies show the log of density and temperature of a shock incident on a clumpy interstellar cloud. The one named nocool is for comparison to demonstrate the effects of radiative cooling. The two files called simply rho and temp are high-res runs with a resolution of 7200x1800 zones. If the name has hydro in it that means that there is a negligible magnetic field.