diff options
Diffstat (limited to 'fg21sim/configs')
| -rw-r--r-- | fg21sim/configs/config.spec | 16 |
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 |