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-rw-r--r--fg21sim/extragalactic/clusters/halo.py25
1 files changed, 23 insertions, 2 deletions
diff --git a/fg21sim/extragalactic/clusters/halo.py b/fg21sim/extragalactic/clusters/halo.py
index 6ecdffa..a21caca 100644
--- a/fg21sim/extragalactic/clusters/halo.py
+++ b/fg21sim/extragalactic/clusters/halo.py
@@ -26,6 +26,10 @@ References
Cassano, Brunetti & Setti, 2006, MNRAS, 369, 1577
http://adsabs.harvard.edu/abs/2006MNRAS.369.1577C
+.. [cassano2007]
+ Cassano et al. 2007, MNRAS, 378, 1565
+ http://adsabs.harvard.edu/abs/2007MNRAS.378.1565C
+
.. [cassano2012]
Cassano et al. 2012, A&A, 548, A100
http://adsabs.harvard.edu/abs/2012A%26A...548A.100C
@@ -205,9 +209,22 @@ class RadioHalo1M:
def radius(self):
"""
The estimated radius of the simulated radio halo.
+
+ 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.
+
+ Reference: Ref.[cassano2007],Sec.4
+
Unit: [kpc]
"""
- return self.f_radius * self.radius_turb(self.t_merger)
+ 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)
@lru_cache()
def radius_strip(self, t_merger):
@@ -771,7 +788,11 @@ class RadioHaloAM(RadioHalo1M):
The halo radius estimated by using the maximum turbulence radius.
Unit: [kpc]
"""
- return self.f_radius * self.radius_turb_max
+ 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)
@property
@lru_cache()