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authorAaron LI <aly@aaronly.me>2017-08-26 23:33:35 +0800
committerAaron LI <aly@aaronly.me>2017-08-26 23:35:35 +0800
commitec2b93030d0077d2598f523dab4f6df8ed2e09b4 (patch)
tree3244ed13dee045223482efc036ca4c91bae4e9fd
parent0f53f6d6a1d3e62d829a21e5ef562de3fa85bb4d (diff)
downloadfg21sim-ec2b93030d0077d2598f523dab4f6df8ed2e09b4.tar.bz2
clusters/halo.py: Update injection rate calculation
The electrons are assumed to be injected throughout the whole cluster ICM/volume.
-rw-r--r--fg21sim/extragalactic/clusters/halo.py15
1 files changed, 5 insertions, 10 deletions
diff --git a/fg21sim/extragalactic/clusters/halo.py b/fg21sim/extragalactic/clusters/halo.py
index 2bd8d59..f24b795 100644
--- a/fg21sim/extragalactic/clusters/halo.py
+++ b/fg21sim/extragalactic/clusters/halo.py
@@ -229,27 +229,22 @@ class RadioHalo:
life (e.g., ``age_obs`` here) is a fraction (``self.eta_e``)
of the total thermal energy of the cluster.
- Note that we assume that the relativistic electrons only permeate
- the halo volume (i.e., of radius ``self.radius``) instead of the
- whole cluster volume (of virial radius).
+ The electrons are assumed to be injected throughout the cluster
+ ICM/volume, i.e., do not restricted inside the halo volume.
Qe(γ) = Ke * γ^(-s),
- int[ Qe(γ) γ me c^2 ]dγ * t_cluster * V_halo =
- eta_e * e_th * V_cluster
+ int[ Qe(γ) γ me c^2 ]dγ * t_cluster = eta_e * e_th
=>
- Ke = [(s-2) * eta_e * e_th * γ_min^(s-2) * (R_vir/R_halo)^3 /
- me / c^2 / t_cluster]
+ Ke = [(s-2) * eta_e * e_th * γ_min^(s-2) / (me * c^2 * t_cluster)]
References
----------
Ref.[cassano2005],Eqs.(31,32,33)
"""
s = self.injection_index
- R_halo = self.radius # [kpc]
- R_vir = helper.radius_virial(self.M_obs, self.z_obs) # [kpc]
e_thermal = helper.density_energy_thermal(self.M_obs, self.z_obs)
term1 = (s-2) * self.eta_e * e_thermal # [erg cm^-3]
- term2 = self.gamma_min**(s-2) * (R_vir/R_halo)**3
+ term2 = self.gamma_min**(s-2)
term3 = AU.mec2 * self.age_obs # [erg Gyr]
Ke = term1 * term2 / term3 # [cm^-3 Gyr^-1]
return Ke