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authorAaron LI <aly@aaronly.me>2019-02-18 22:33:39 +0800
committerAaron LI <aly@aaronly.me>2019-02-18 22:38:07 +0800
commit27dc87774ad6f63ed4ba68201bdfe7b9b4ca2587 (patch)
tree6033407d177b7a34824da7c765b021979bd15e5d
parent0de191f82ffbb981501da4de96b83ad01971a4c2 (diff)
downloadfg21sim-27dc87774ad6f63ed4ba68201bdfe7b9b4ca2587.tar.bz2
clusters/halo: Further extend the halo radius calculation
-rw-r--r--fg21sim/configs/config.spec6
-rw-r--r--fg21sim/extragalactic/clusters/halo.py23
2 files changed, 15 insertions, 14 deletions
diff --git a/fg21sim/configs/config.spec b/fg21sim/configs/config.spec
index 1bfb27a..556c662 100644
--- a/fg21sim/configs/config.spec
+++ b/fg21sim/configs/config.spec
@@ -397,9 +397,13 @@ stream = option("stderr", "stdout", "", default="stderr")
x_cr = float(default=0.015, min=0.001, max=0.1)
# The scaling index of the diffusion coefficient (D_γγ) w.r.t. the
- # mass of the main cluster.
+ # mass of the cluster.
mass_index = float(default=0, min=0, max=2)
+ # The scaling index of the halo radius (R_halo) w.r.t. the virial
+ # radius of the cluster.
+ radius_index = float(default=0, min=0, max=3)
+
# The spectral index of the injected primary electrons.
injection_index = float(default=2.3, min=2.1, max=3.0)
diff --git a/fg21sim/extragalactic/clusters/halo.py b/fg21sim/extragalactic/clusters/halo.py
index a21caca..cc90c7a 100644
--- a/fg21sim/extragalactic/clusters/halo.py
+++ b/fg21sim/extragalactic/clusters/halo.py
@@ -160,6 +160,7 @@ class RadioHalo1M:
self.x_cr = configs.getn(sec+"/x_cr")
self.eta_b = self.x_cr # Equipartition between magnetic field and CR
self.mass_index = configs.getn(sec+"/mass_index")
+ self.radius_index = configs.getn(sec+"/radius_index")
self.gamma_min = configs.getn(sec+"/gamma_min")
self.gamma_max = configs.getn(sec+"/gamma_max")
self.gamma_np = configs.getn(sec+"/gamma_np")
@@ -212,19 +213,16 @@ class RadioHalo1M:
It is known that the halo radius scales non-linearly as the hosting
cluster, breaking the self-similiarity, which may be caused by the
- magnetic field and the releativistic electron distributions. So
- make the halo radius scales with the magnetic field.
+ magnetic field and the releativistic electron distributions.
Reference: Ref.[cassano2007],Sec.4
Unit: [kpc]
"""
- r = self.radius_turb(self.t_merger)
- B = helper.magnetic_field(mass=self.M_obs, z=self.z_obs,
- eta_b=self.eta_b, kT_out=self.kT_out)
- B0 = helper.magnetic_field(mass=1e15, z=0,
- eta_b=self.eta_b, kT_out=self.kT_out)
- return r * self.f_radius * (B/B0)
+ r_turb = self.radius_turb(self.t_merger)
+ r_cl = helper.radius_cluster(mass=self.M_obs, z=self.z_obs)
+ r0_cl = helper.radius_cluster(mass=1e15, z=0)
+ return r_turb * self.f_radius * (r_cl/r0_cl)**self.radius_index
@lru_cache()
def radius_strip(self, t_merger):
@@ -788,11 +786,10 @@ class RadioHaloAM(RadioHalo1M):
The halo radius estimated by using the maximum turbulence radius.
Unit: [kpc]
"""
- B = helper.magnetic_field(mass=self.M_obs, z=self.z_obs,
- eta_b=self.eta_b, kT_out=self.kT_out)
- B0 = helper.magnetic_field(mass=1e15, z=0,
- eta_b=self.eta_b, kT_out=self.kT_out)
- return self.f_radius * self.radius_turb_max * (B/B0)
+ r_turb = self.radius_turb_max
+ r_cl = helper.radius_cluster(mass=self.M_obs, z=self.z_obs)
+ r0_cl = helper.radius_cluster(mass=1e15, z=0)
+ return r_turb * self.f_radius * (r_cl/r0_cl)**self.radius_index
@property
@lru_cache()