diff options
| author | Aaron LI <aly@aaronly.me> | 2018-01-16 09:23:52 +0800 |
|---|---|---|
| committer | Aaron LI <aly@aaronly.me> | 2018-01-16 09:23:52 +0800 |
| commit | 1200e50fd24451ed7b56d137a20106c18c0e0153 (patch) | |
| tree | ef73efe9315e8774556f3215ccf523b51c609b37 | |
| parent | 8dcf5caa1e6b37d7717ea04167e96ebee3e9516a (diff) | |
| download | fg21sim-1200e50fd24451ed7b56d137a20106c18c0e0153.tar.bz2 | |
clusters: minor updates
| -rw-r--r-- | fg21sim/configs/20-extragalactic.conf.spec | 2 | ||||
| -rw-r--r-- | fg21sim/extragalactic/clusters/helper.py | 9 |
2 files changed, 6 insertions, 5 deletions
diff --git a/fg21sim/configs/20-extragalactic.conf.spec b/fg21sim/configs/20-extragalactic.conf.spec index cb11bd8..7de9eb1 100644 --- a/fg21sim/configs/20-extragalactic.conf.spec +++ b/fg21sim/configs/20-extragalactic.conf.spec @@ -132,6 +132,8 @@ # 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 diff --git a/fg21sim/extragalactic/clusters/helper.py b/fg21sim/extragalactic/clusters/helper.py index 39cee12..8d6db09 100644 --- a/fg21sim/extragalactic/clusters/helper.py +++ b/fg21sim/extragalactic/clusters/helper.py @@ -2,7 +2,7 @@ # MIT license """ -Helper functions +Functions to help simulate galaxy cluster diffuse emissions. References ---------- @@ -295,8 +295,7 @@ def speed_sound(kT): Reference: Ref.[zhuravleva2014],Appendix(Methods) """ - # The gas adiabatic index - gamma = AC.gamma + gamma = AC.gamma # gas adiabatic index cs = np.sqrt(gamma * kT*AUC.keV2erg / (AC.mu * AC.u)) # [cm/s] return cs * AUC.cm2km # [km/s] @@ -377,12 +376,12 @@ def time_crossing(M_main, M_sub, z=0.0): def time_turbulence(M_main, M_sub, z=0.0, configs=CONFIGS): """ - The timescale that the compressive turbulence persists, which is + The duration that the compressive turbulence persists, which is estimated as: τ_turb ≅ 2*d / v_impact, where d ≅ L ≅ R_vir / 3, and L is also the turbulence injection scale. - During this timescale, the merger-induced turbulence is regarded + During this period, the merger-induced turbulence is regarded to accelerate the relativistic electrons effectively. Unit: [Gyr] |