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* clusters/mergertree: import matplotlib only when usedAaron LI2018-01-011-4/+6
| | | | In this way to avoid dependency on matplotlib. Also add print messages.
* clusters/mergertree: improve print formats for "show_mtree()"Aaron LI2018-01-011-4/+7
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* Minor changesAaron LI2018-01-011-22/+22
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* clusters/formation: Move parameter "ratio_major" to recent_major_merger()Aaron LI2018-01-012-32/+19
| | | | | | * Simplify "max_merger" property to not check whether it is a major merger. * Rename "max_merger" to "maximum_merger" * Rename "simulate_mergertree()" to "simulate_mtree()"
* clusters/halo: Change option "tau_merger" to "time_traceback"Aaron LI2018-01-011-4/+4
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* clusters/halo: adjust radio halo size estimationAaron LI2018-01-011-3/+3
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* clusters/halo: improve turbulence velocity dispersion calculationAaron LI2018-01-011-9/+9
| | | | | | | Use the merged total mass instead of the main cluster mass only as the denominator to determine the turbulence velocity dispersion, which reduces the scatter and thus the acceleration results will be less sensitive to the (mostly unknown) merging turbulence properties.
* clusters/halo: Add back "mach_turbulence" attributeAaron LI2017-12-312-4/+15
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* clusters/halo: Rework the turbulence acceleration timescale calculationAaron LI2017-12-311-47/+39
| | | | | | | | The new method adopted to determine the turbulence acceleration timescale follows [miniati2015] and [pinzke2017], in which the merger-induced turbulence cascades into small scales (and thus accelerate electrons) through the TTD (transit-time damping) mechanism by scattering mainly with the relativistic particles (cosmic-ray protons and electrons).
* clusters/halo: calc turbulence velocity dispersion based on mergerAaron LI2017-12-311-0/+38
| | | | | Also update the description of option "extragalactic/halos/eta_turb" and change its default value to 0.1
* clusters/halo/helper: Add fmass_nfw() to calc NFW mass profileAaron LI2017-12-311-0/+30
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* Minor cleanupsAaron LI2017-12-311-3/+7
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* Minor cleanupsAaron LI2017-12-301-4/+4
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* clusters/halo: support to drop out the most powerful halosAaron LI2017-12-301-0/+26
| | | | | The new option "extragalactic/clusters/halo_dropout" is added to specify how many halos to be dropped out.
* clusters/halo: Add virial_speed() helper functionAaron LI2017-12-301-2/+13
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* clusters/halo: Estimate turbulence acceleration w.r.t. injection scaleAaron LI2017-12-303-16/+39
| | | | The turbulence injection scale ~ halo size
* cluster/halo: Estimate halo radius ~ 0.33*R_vir (main cluster)Aaron LI2017-12-302-8/+17
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* clusters/halo: Tune the maximum acceleration timescale to 10 GyrAaron LI2017-11-161-6/+17
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* clusters/halo: improve advection calculationAaron LI2017-11-161-10/+10
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* Update logging messagesAaron LI2017-10-291-0/+2
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* clusters/configs: Update f_acc default to 1.0; also update descriptionsAaron LI2017-10-261-1/+1
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* clusters/halo: Calc turbulence injection scale w.r.t. sub-cluster radiusAaron LI2017-10-261-6/+8
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* clusters/solver: Update buffer_np description and handlingAaron LI2017-10-252-4/+11
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* clusters/solver: Remove an empty methodAaron LI2017-10-251-8/+0
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* clusters/halo: Fix fp_advection() w.r.t. initial electron spectrum calc.Aaron LI2017-10-251-2/+4
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* clusters/halo: Adjust initial electron spectrum calculationAaron LI2017-10-251-4/+6
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* clusters/halo: Add method to derive the initial electron spectrumAaron LI2017-10-251-11/+51
| | | | | Also add the option "time_init" to control how long a period is used to derive the initial electron spectrum.
* clusters/halo: Fix passing the "configs" objectAaron LI2017-10-252-4/+6
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* clusters/halo: Always pass the using configsAaron LI2017-10-242-9/+12
| | | | | The user-using `configs` object may be different to the global `CONFIGS`, which may be forgotten to load the up-to-date user configurations.
* clusters/halo: Change zbegin/zend to tstart/tsop (use cosmic time)Aaron LI2017-10-241-19/+20
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* clusters/halo: Add method "_magnetic_field()"Aaron LI2017-10-241-2/+23
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* clusters/halo: Rename property "magnetic_field" to "B_obs"Aaron LI2017-10-242-4/+4
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* clusters/halo: Allow specify magnetic field in calc_emissivity()Aaron LI2017-10-241-9/+14
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* clusters/halos: Fix halo radius calculationAaron LI2017-10-231-3/+5
| | | | Also change the parameter "nr" default to 2.0 for draw_halo() function.
* clusters/psformalism: Use functools.lru_cache()Aaron LI2017-10-231-0/+3
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* clusters/halo: merge halo_rprofile() & draw_halo(); Fix halo radius errorAaron LI2017-10-232-40/+28
| | | | | | | * Fix the error that misses to divide the halo radius by 3 for the e-folding radius, which causes the generated halo image has a 3x size! * Merge function "halo_rprofile()" into "draw_halo()" * Skip transform circular halo into elliptical one if "felong" is None
* clusters/halo: Use "lru_cache()", also improves some performanceAaron LI2017-10-233-13/+26
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* clusters/formation: Fix problem that no mergers occurredAaron LI2017-10-222-2/+9
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* clusters/halo: Add "use_max_merger" option to allow use max merger eventsAaron LI2017-10-221-20/+30
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* clusters/formation: Add method to found the maximum merger eventAaron LI2017-10-221-1/+51
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* clusters/halo: Add option "kT_out" to tune cluster temperatureAaron LI2017-10-222-5/+7
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* clusters/halo: Rewrite turbulence acceleration & diffusion coefficient!Aaron LI2017-10-212-58/+92
| | | | | | | | | | | | The previous calculation of the turbulence acceleration efficiency has significant problems, which is too low, i.e., the acceleration timescale is too large (~10 Gyr). However, it is reported that turbulent acceleration has a timescale ~100 Myr (0.1 Gyr). I believe this problem is due to the over-simplification to the formula proposed by [cassano2005]. Rewrite the turbulence acceleration and diffusion coefficient calculations, adopting the method proposed by [brunetti2016]. To this end, two new options "f_lturb" and "f_acc" are introduced to tune the results.
* clusters/halos: Add more cluster and halo propertiesAaron LI2017-10-212-12/+39
| | | | | | * Rvir0, Rvir_main, Rvir_sub * kT_main, kT_sub (replace kT_merger) * radius -> Rhalo, angular_radius -> Rhalo_angular, B -> B0
* clusters: Fix a comment about "felong"Aaron LI2017-10-211-2/+1
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* clusters/halo: Add function "speed_sound()"Aaron LI2017-10-211-0/+28
| | | | Also add "gamma" the adiabatic index of ideal gas to utils/units.py
* clusters/halo: Determine magnetic field by fraction of its energy densityAaron LI2017-10-202-32/+26
| | | | | | | | | | * Rewrite "magnetic_field()" function to calculate the mean magnetic field strength within ICM according its energy density fraction w.r.t. the ICM thermal energy density. * Remove config options "b_mean" and "b_index", which are replaced with the option "eta_b", the assumed magnetic energy density fraction w.r.t. the ICM thermal energy density.
* clusters/halo: Remove "mass_to_kT()", replaced by "kT_cluster()"Aaron LI2017-10-201-39/+0
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* clusters/halo: Add "kT_obs" and "tback_merger" propertiesAaron LI2017-10-192-2/+19
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* clusters/halo: Use "kT_cluster()" instead of "mass_to_kT()"Aaron LI2017-10-192-4/+4
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* clusters/halo: Add kT_cluster() to calculate the cluster ICM temperatureAaron LI2017-10-191-0/+25
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