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Central_object Parameters
A booliean variable stating whether of not the central object should radiate. This will enable different follow-up questions depending on the system type (AGN/non-AGN).
Boolean (yes/no)
-
System_type:
star
,binary
,previous
,agn
File: setup_star_bh.c
If the central source in an AGN/BH system is radiating, what geometry should it radiate from? This is applicable even for black-body sources, where the luminosity depends on Central_object.radius.
Enumerator
-
lamp_post
: The central source radiates from two point sources located on the system axis above and below the disk plane. Emission is completely isotropic. -
sphere
: The central source radiates from a spherical surface with radius Central_object.radius. Emission is cosine-weighted in the direction of the sphere normal at the point of emission. Photons that would be spawned in an extended disk (if Disk.type isvertically.extended
) are re-generated.
-
System_type:
agn
-
Central_object.radiation:
True
File: setup_star_bh.c
The distance above and below the disk plane of the two point sources used in the lamp-post model.
Double
Greater than 0
-
Central_object.geometry_for_source:
lamp_post
File: setup_star_bh.c
This is a command to define a cloudy type broken power law SED - mainly used for testing the code against cloudy. This SED has hardwired frequency exponents of 2.5 below the low energy break and -2.0 above the high energy break. This parameter defines the energy of the low energy break.
Double
eV
Greater than 0
-
Central_object.radiation:
True
File: setup_star_bh.c
This is a command to define a cloudy type broken power law SED - mainly used for testing the code against cloudy. This SED has hardwired frequency exponents of 2.5 below the low energy break and -2.0 above the high energy break. This parameter defines the energy of the high energy break.
Double
eV
Greater than Central_object.cloudy.low_energy_break
-
System_type:
agn
-
Central_object.radiation:
True
File: setup_star_bh.c
Determines the SED of the central object in the spectral cycles. The luminosity is set by the options for the ionisation cycles, however.
Enumerator
-
bb
: Available for System_type ofstar
orbinary
. Black-body radiation. The boundary layer radiates as a black-body source with surface luminosity set by its effective temperature (Central_object.temp) and resulting in a total luminosity proportional to its surface area. -
models
: Available for System_type ofstar
orbinary
. Radiate according to a model. Python can support tabulated models that output with a binned luminosity distribution depending on system properties like temperature and gravity. See Input_spectra.model_file. The total luminosity will be set by Central_object.luminosity. -
uniform
: Available for System_type ofstar
orbinary
. Photons are generated with a random, uniformly-distributed wavelength between Spectrum.wavemin and Spectrum.wavemax. Can in some cases substitute for a Kurcuz spectrum. This mode is only available when generating final spectra. -
brems
: Available for System_type ofagn
only. Central object radiates with SED of a brehmsstralung spectrum as . This was originally developed to allow comparison to spectra generated according to Blondin heating and cooling rates. -
cloudy
: Available for System_type ofagn
only. Central object radiates with a 'broken' power law, intended largely for testing purposes against Cloudy. The SED form is , but beyond the provided high and low energy breakpoints the luminosity falls off sharply. -
power
: Available for System_type ofagn
only. Radiate following a power-law model as . The total luminosity will be set by Boundary_layer.luminosity.
-
Central_object.radiation:
True
File: python.c
The luminosity of a non-blackbody AGN central source. This is defined as the luminosity from 2-10keV.
Double
ergs/s
Greater than 0.
-
System_type:
agn
-
Central_object.radiation:
True
-
Central_object.rad_type_to_make_wind:
brems
,cloudy
,model
,power
File: setup_star_bh.c
Temperature of the central star. Physically, this is used in blackbody radiation, shock heating and disk heating in YSO models. It is also used to help determine the frequency bands in which photons are emitted.
Double
Kelvin
Greater than zero
-
System_type:
star
,binary
,previous
File: setup_star_bh.c
Multi-line description, must keep indentation.
Enumerator
-
bb
: Available for System_type ofstar
orbinary
. Black-body radiation. The boundary layer radiates as a black-body source with surface luminosity set by its effective temperature (Central_object.temp) and resulting in a total luminosity proportional to its surface area. -
models
: Available for System_type ofstar
orbinary
. Radiate according to a model. Python can support tabulated models that output with a binned luminosity distribution depending on system properties like temperature and gravity. See Input_spectra.model_file. The total luminosity will be set by Central_object.luminosity. -
brems
: Available for System_type ofagn
only. Central object radiates with SED of a brehmsstralung spectrum as . This was originally developed to allow comparison to spectra generated according to Blondin heating and cooling rates. -
cloudy
: Available for System_type ofagn
only. Central object radiates with a 'broken' power law, intended largely for testing purposes against Cloudy. The SED form is , but beyond the provided high and low energy breakpoints the luminosity falls off sharply. -
power
: Available for System_type ofagn
only. Radiate following a power-law model as . The total luminosity will be set by Boundary_layer.luminosity.
File: setup_star_bh.c
Adds a low-frequency cutoff to the power law spectrum.
Whilst this is required for power-law emission modes,
it's set globally and also used in cloudy
broken-power-law emission modes!
Double
Hz
Greater than or equal to 0
File: setup_star_bh.c
The frequency exponent 𝛼 in bremstrahlung SED of the form
Double
Any - sign is not assumed so use negative if you want negative
File: setup_star_bh.c
The temperature T in bremstrahlung SED of the form
Double
K
Greater than 0
File: setup_star_bh.c
If the AGN/BH is radiating as a black body, what temperature should it radiate at?
Double
Kelvin
Greater than 0
File: setup_star_bh.c
The exponent 𝛼 in a power law SED applied to a power law source of the form .
See Radiation_types and Boundary_layer.power_law_index.
Double
Greater than 0
-
Central_object.rad_type_to_make_wind:
cloudy
,power
File: setup_star_bh.c
Mass of the central object. This is very important, affecting wind speeds, gravitational heating and such.
Double
M☉
Greater than 0
File: setup_star_bh.c
Radius of the central object in the system, e.g the white dwarf or black hole
Double
cm
Greater than 0
File: setup_star_bh.c