Commit 3aac6968 authored by Matthieu Schaller's avatar Matthieu Schaller
Browse files

Merge branch 'Cooling-Halo-Updates' into 'master'

Cooling halo updates

Small update to README for generating videos from snapshots and update to `test_energy` script to be able to run with any number of snapshots.

See merge request !286
parents 2474a3c2 7647d519
Initial Conditions Generation
To make the initial conditions we distribute gas particles randomly in
a cube with a side length twice that of the virial radius. The density
profile of the gas is proportional to r^(-2) where r is the distance
......@@ -16,14 +17,31 @@ While the system is initially in hydrostatic equilibrium, the cooling
of the gas and the non-zero angular momentum means that the halo will
collapse into a spinning disc.
To run this example, make such that the code is compiled with either
the isothermal potential or softened isothermal potential, and
'const_lambda' cooling, set in src/const.h. In the latter case, a
(small) value of epsilon needs to be set in cooling.yml. 0.1 kpc
should work well.
Checking Results
The plotting scripts produce a plot of the density, internal energy
and radial velocity profile for each
snapshot. shows the evolution of energy
with time. These can be used to check if the example has run properly.
Generating Video
If you want to generate a video of the simulation, the frequency of
the snaphots needs to be increased. This can be modified in cooling.yml
by changing 'delta_time' to 0.01.
Once you have the snapshots, 'gadgetviewer' can be used to create a
series of snapshot frames. The frames can then be combined together with
'ffmpeg' to produce a video. The following command can be used:
ffmpeg -r 20 -i frame_%05d.image.png -c:v ffv1 -qscale:v 0 movie.avi
to produce the video.
......@@ -2,8 +2,11 @@ import numpy as np
import h5py as h5
import matplotlib.pyplot as plt
import sys
import glob
n_snaps = 101
# Get the total number of snapshots
file_list = glob.glob("CoolingHalo_*")
n_snaps = len(file_list)
#some constants
OMEGA = 0.3 # Cosmological matter fraction at z = 0
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