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Central_object Parameters

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Sam Mangham edited this page Jul 12, 2019 · 4 revisions

Central_object.radiation

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).

Type

Boolean (yes/no)

Parent(s)

File: setup_star_bh.c

Central_object.geometry_for_source

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.

Type

Enumerator

Values

  • 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 is vertically.extended) are re-generated.

Parent(s)

File: setup_star_bh.c

Central_object.lamp_post_height

The distance above and below the disk plane of the two point sources used in the lamp-post model.

Type

Double

Unit

Central_object.radius

Values

Greater than 0

Parent(s)

File: setup_star_bh.c

Central_object.cloudy.low_energy_break

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.

Type

Double

Unit

eV

Values

Greater than 0

Parent(s)

File: setup_star_bh.c

Central_object.cloudy.high_energy_break

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.

Type

Double

Unit

eV

Values

Greater than Central_object.cloudy.low_energy_break

Parent(s)

File: setup_star_bh.c

Central_object.rad_type_in_final_spectrum

Determines the SED of the central object in the spectral cycles. The luminosity is set by the options for the ionisation cycles, however.

Type

Enumerator

Values

  • bb: Available for System_type of star or binary. 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 of star or binary. 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 of star or binary. 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 of agn only. Central object radiates with SED of a brehmsstralung spectrum as L_\nu=\nu^{\alpha}e^{-h\nu/kT}. This was originally developed to allow comparison to spectra generated according to Blondin heating and cooling rates.

  • cloudy: Available for System_type of agn only. Central object radiates with a 'broken' power law, intended largely for testing purposes against Cloudy. The SED form is L_\nu=K\nu^\alpha, but beyond the provided high and low energy breakpoints the luminosity falls off sharply.

  • power: Available for System_type of agn only. Radiate following a power-law model as L_\nu=K\nu^\alpha. The total luminosity will be set by Boundary_layer.luminosity.

Parent(s)

File: python.c

Central_object.luminosity

The luminosity of a non-blackbody AGN central source. This is defined as the luminosity from 2-10keV.

Type

Double

Unit

ergs/s

Values

Greater than 0.

Parent(s)

File: setup_star_bh.c

Central_object.temp

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.

Type

Double

Unit

Kelvin

Values

Greater than zero

Parent(s)

File: setup_star_bh.c

Central_object.rad_type_to_make_wind

Multi-line description, must keep indentation.

Type

Enumerator

Values

  • bb: Available for System_type of star or binary. 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 of star or binary. 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 of agn only. Central object radiates with SED of a brehmsstralung spectrum as L_\nu=\nu^{\alpha}e^{-h\nu/kT}. This was originally developed to allow comparison to spectra generated according to Blondin heating and cooling rates.

  • cloudy: Available for System_type of agn only. Central object radiates with a 'broken' power law, intended largely for testing purposes against Cloudy. The SED form is L_\nu=K\nu^\alpha, but beyond the provided high and low energy breakpoints the luminosity falls off sharply.

  • power: Available for System_type of agn only. Radiate following a power-law model as L_\nu=K\nu^\alpha. The total luminosity will be set by Boundary_layer.luminosity.

File: setup_star_bh.c

Central_object.power_law_cutoff

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!

Type

Double

Unit

Hz

Values

Greater than or equal to 0

Parent(s)

File: setup_star_bh.c

Central_object.bremsstrahlung_alpha

The frequency exponent 𝛼 in bremstrahlung SED of the form L_\nu=\nu^{}\alpha}e^{-h\nu/kT}

Type

Double

Values

Any - sign is not assumed so use negative if you want negative

Parent(s)

File: setup_star_bh.c

Central_object.bremsstrahlung_temp

The temperature T in bremstrahlung SED of the form L_\nu=\nu^{\alpha}e^{-h\nu/kT}

Type

Double

Unit

K

Values

Greater than 0

Parent(s)

File: setup_star_bh.c

Central_object.blackbody_temp

If the AGN/BH is radiating as a black body, what temperature should it radiate at?

Type

Double

Unit

Kelvin

Values

Greater than 0

Parent(s)

File: setup_star_bh.c

Central_object.power_law_index

The exponent 𝛼 in a power law SED applied to a power law source of the form L_\nu=K\nu^\alpha.

See Radiation_types and Boundary_layer.power_law_index.

Type

Double

Values

Greater than 0

Parent(s)

File: setup_star_bh.c

Central_object.mass

Mass of the central object. This is very important, affecting wind speeds, gravitational heating and such.

Type

Double

Unit

M☉

Values

Greater than 0

File: setup_star_bh.c

Central_object.radius

Radius of the central object in the system, e.g the white dwarf or black hole

Type

Double

Unit

cm

Values

Greater than 0

File: setup_star_bh.c

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