diff options
| -rw-r--r-- | fg21sim/extragalactic/clusters/halo.py | 15 |
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 |