wiki:1DRadShocks

Version 3 (modified by ehansen, 12 years ago) ( diff )

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1D Radiative Shocks

These simulations follow Ch. 4 of Delamarter '01 and his treatment of the 1D steady radiative shock problem. The purpose of this problem is to check that the cooling source terms are being handled correctly. Here are some useful links:

AstroBEAR 1.0 test page

Delamarter '01 pdf

Equations

The shock jump equations for a stationary shock are used to solve for the initial post-shock values. The post-shock velocity v2 can be written as:

where v1 is the ambient velocity, and M is the ambient mach number. Remember that the mach number M = v1/c where c is the ambient sound speed, and where P1 is ambient pressure, and is ambient density. The post-shock density and pressure ( and P2 respectively) can be found by using mass flux and momentum flux conservation across the shock:

These post-shock values become the boundary conditions for the fluid equations in the cooling region:

where , v, and P represent the density, velocity, and pressure in the cooling region as functions of x, and is the cooling rate.


Initial Parameters

n1 = 60 particles/cc

v1 = 107 cm/s

T1 = 104 K

For analytic cooling,

where n and T and the number density and temperature in the post-shock region respectively.

For these simulations,

= 2

= 1.23786 * 10-34 erg*cm3/s/K2

cell length = 2.5 x 1015 cm

problem domain = 400 cells

final time ~ 4000 years


Results

A run with no cooling was done to make sure the post-shock values were correct. With no cooling (adiabatic), the hydrodynamic quantities should jump discontinuously at the shock, and then remain constant while the shock itself remains stationary. Only the first 100 cells of the simulation are shown here.

Adiabatic
Pressure Movie Temperature Movie
Density Movie Velocity Movie

Then, a run with the aforementioned analytic cooling parameters was done. The hydrodynamic quantities will change discontinuously at the shock as before, but then change continuously according to the cooling rate. The ambient temperature is set to be the floor temperature, so that no cooling occurs at or below this temperature. Once the post-shock temperature reaches this floor temperature, the hydrodynamic quantities will remain constant. This is called the quiescent region. Only the first 100 cells of the simulation are shown here.

Analytic Cooling
Pressure Movie Temperature Movie
Density Movie Velocity Movie

For Dalgarno-McCray (DM) cooling, some of the initial parameters had to be changed. The initial velocity used in the previous simulations would give rise to a post-shock temperature in the unstable region of the DM curve. This led to the radiative instability, and thus unsteady shocks. To avoid this, the initial velocity was lowered to 80 km/s. Also, the cooling rate from the DM curve is much higher than that of the analytic form. In order to see the cooling region, the grid had to be shrunk, resulting in a cell length of 1013 cm.

DM Cooling
Temperature Movie

For Non-equilibrium (NEQ) cooling, the length scale had to be adjusted. The shock velocity is the same as the DM case, but the cell length is now 7.75e11 cm.

NEQ Cooling
No image "NEQ_temp0010.png" attached to 1DRadShocks
Temperature Movie

Z Cooling has the same initial parameters and scaling as the NEQ case.

Z Cooling
No image "Z_temp0010.png" attached to 1DRadShocks
Temperature Movie

Here is a fun plot that shows the temperature profiles for DM, NEQ, and Z cooling. This gives you a good idea of the temperature ranges that each type of cooling works in. Also, you can see the differences in the cooling length which is why I would normally change the length scale depending on the type of cooling.


Including MHD

Making these simulations work with MHD was no simple task. Having a magnetic field adds another jump condition, and it makes the equations within the cooling region more complicated. Here are what the equations look like now:

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