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authorAaron LI <aly@aaronly.me>2017-08-01 00:13:54 +0800
committerAaron LI <aly@aaronly.me>2017-08-01 00:13:54 +0800
commit85add9c303161f4a68c15a495ef1fc8af8182635 (patch)
tree5ad10aa28551fd1e3ee7f72a47f99cf30d0b53a4 /fg21sim
parentc75dfd265e82b62af330f29be492a35c831238cc (diff)
downloadfg21sim-85add9c303161f4a68c15a495ef1fc8af8182635.tar.bz2
clusters/halo.py: Finished brief simulation description
Diffstat (limited to 'fg21sim')
-rw-r--r--fg21sim/extragalactic/clusters/halo.py16
1 files changed, 13 insertions, 3 deletions
diff --git a/fg21sim/extragalactic/clusters/halo.py b/fg21sim/extragalactic/clusters/halo.py
index 50c1242..586c7e0 100644
--- a/fg21sim/extragalactic/clusters/halo.py
+++ b/fg21sim/extragalactic/clusters/halo.py
@@ -68,9 +68,19 @@ class RadioHalo:
only during merger crossing), and then been disabled (i.e.,
only radiation and ionization losses later);
3. Assume the electrons are constantly injected and has a power-law
- energy spectrum;
- 4. Determine the initial electron density
- TODO...
+ energy spectrum, determine the injection rate by further assuming
+ that the total injected electrons has energy of a fraction (eta_e)
+ of the ICM total thermal energy;
+ 4. Set the initial electron density/spectrum be the total injected
+ electrons during t_merger time;
+ 5. Calculate the magnetic field from the cluster total mass (which
+ is assumed to be growth linearly from M_main+M_sub to M_obs);
+ 6. Calculate the energy losses for the coefficients of Fokker-Planck
+ equation;
+ 7. Solve the Fokker-Planck equation to derive the relativistic
+ electron spectrum at t_obs (i.e., z_obs);
+ 8. Calculate the synchrotron emissivity from the derived electron
+ spectrum.
Parameters
----------