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-rw-r--r--fg21sim/configs/config.spec16
1 files changed, 3 insertions, 13 deletions
diff --git a/fg21sim/configs/config.spec b/fg21sim/configs/config.spec
index d580d3f..1ba8dd3 100644
--- a/fg21sim/configs/config.spec
+++ b/fg21sim/configs/config.spec
@@ -354,13 +354,6 @@ stream = option("stderr", "stdout", "", default="stderr")
# Unit: [Gyr]
time_traceback = float(default=3.0, min=1.0, max=5.0)
- # The fraction of the magnetic field energy density w.r.t. the ICM
- # thermal energy density, which is used to determine the mean magnetic
- # field strength within the ICM and is also assumed to be uniform.
- # * ~< 0.4% (Ref: Pfrommer & Ensslin 2004, MNRAS)
- # * ~0.3%-1% (Ref: Bohringer et al. 2016, A&A)
- eta_b = float(default=0.001, min=1e-5, max=0.1)
-
# The temperature of the outer gas surrounding the cluster. Accretion
# shocks form near the cluster virial radius during the cluster formation,
# which can heat the cluster ICM to have a higher temperature than the
@@ -401,12 +394,9 @@ stream = option("stderr", "stdout", "", default="stderr")
# electrons during the cluster life time.
eta_e = float(default=0.003, min=0.001, max=0.1)
- # The ratio of cosmic ray (including protons and electrons) energy
- # density (i.e., pressure) to the thermal energy density.
- # NOTE: Fermi-LAT has placed an upper limit of ~1.25%-1.4%
- # (Ackermann et al. 2014, ApJ, 787, 18)
- # NOTE: The energy ratio of cosmic-ray electrons to protons K_ep ~0.01
- # for our Galaxy (Pinzke et al. 2017, MNRAS, 465, 4800)
+ # The energy density ratio of cosmic ray to the thermal ICM.
+ # NOTE: Equipartition between the magnetic field and cosmic ray is
+ # assumed, i.e., eta_b == x_cr.
x_cr = float(default=0.015, min=0.001, max=0.1)
# Electron injection, which is assumed to have a constant injection