| Commit message (Collapse) | Author | Age | Files | Lines |
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Remove the obsolete options: ratio_major, use_max_merger
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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).
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Also update the description of option "extragalactic/halos/eta_turb"
and change its default value to 0.1
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The new option "extragalactic/clusters/halo_dropout" is added to specify how
many halos to be dropped out.
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* Update the __init__ description a bit
* Add the missing parameter change for ``f_acc``
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Also add the option "time_init" to control how long a period is used to derive
the initial electron spectrum.
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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.
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* 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.
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Add option "use_dump_halos_data" to control whether to just use the previously
dumped halos data, therefore, the radio emissions at additional frequencies
can be simply calculated.
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Replace option "halos_dumpfile" with "halos_catalog_outfile", and use
option "dump_halos_data" to control whether to dump the raw data.
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* New dependency "hmf" (halo mass functions) module
* Calculate halo mass distributions/functions (dndlnm) with respect to masses
and redshifts, instead of use the previous data file ("ps_data")
* New section "[extragalactic][psformalism]" in configurations
* New functions to write and read the dndlnm data
TODO:
* update the method to sample (mass, redshift) for clusters from the dndlnm
data
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NOTE:
The cluster number (especially the bright ones) may be rather small
within a sky patch. This ``boost`` config option increase the expected
cluster number by a specified times, for better testing purpose.
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Carried many simulation tests to determine the best parameters, by
comparing with the integrated counts distribution (i.e., halo luminosity
function) reported in previous works (Cassano2006, Cassano2012, and
Ensslin2002).
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Use "1 - baryon_fraction = 1 - Ob0/Om0" to replace "f_darkmatter".
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* Adopt the electron acceleration coefficient formula from [cassano2005]
* Rename method "_tau_acceleration()" to "_chi_acceleration()", and
rewrite
* Add property "kT_merger"
* Also save "kT_merger" and "chi" into halos data
Signed-off-by: Aaron LI <aly@aaronly.me>
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Signed-off-by: Aaron LI <aly@aaronly.me>
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Signed-off-by: Aaron LI <aly@aaronly.me>
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Also updated configuration options.
Signed-off-by: Aaron LI <aly@aaronly.me>
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This makes the simulation agree better with observations,
e.g., <Jsyn> ~ 1e-42 [erg/s/cm^3/Hz]
Signed-off-by: Aaron LI <aly@aaronly.me>
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Signed-off-by: Aaron LI <aly@aaronly.me>
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This configuration option "beta_turb" has different meaning as
"eta_turb" in [Cassano & Brunetti 2005], though they can both be an
indicator for the turbulence acceleration efficiency.
Rename this configuration option to make the difference more clear.
Signed-off-by: Aaron LI <aly@aaronly.me>
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Signed-off-by: Aaron LI <aly@aaronly.me>
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And update the config specification accordingly with some cleanups.
Signed-off-by: Aaron LI <aly@aaronly.me>
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Also update the configurations
Signed-off-by: Aaron LI <aly@aaronly.me>
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Simulate the formation history of each cluster and identify the
last/recent major merger event.
Also add new configuration option "tau_merger" and tweak several
configurations options.
Signed-off-by: Aaron LI <aly@aaronly.me>
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