hyperion.dust.IsotropicDust

class hyperion.dust.IsotropicDust(nu, albedo, chi)

This class should be used for dust properties that include isotropic scattering. The dust properties should be instatiated as:

d = IsotropicDust(nu, albedo, chi)

where nu, albedo, and chi are 1-D Numpy arrays containing the frequencies, albedo, and opacity to extinction respectively.

Method

set_sublimation_temperature(mode[, temperature]) Set the dust sublimation mode and temperature.
set_sublimation_specific_energy(mode[, …]) Set the dust sublimation mode and specific energy.
set_lte_emissivities([n_temp, temp_min, …]) Calculate the emissivities assuming LTE
plot(filename)
read(filename) Read in from a standard dust file
write(filename[, compression]) Write out to a standard dust file, including calculations of the mean opacities and optionally thermal emissivities.
temperature2specific_energy(temperature) Convert a temperature to its corresponding specific energy value.
specific_energy2temperature(specific_energy) Convert a specific energy value to its corresponding temperature.
chi_nu_temperature(temperature) Compute the mean opacity to extinction for a blackbody at a given temperature.
kappa_nu_temperature(temperature) Compute the mean opacity to absorption for a blackbody at a given temperature.
chi_nu_spectrum(nu, fnu) Compute the mean opacity to extinction for a given spectrum.
kappa_nu_spectrum(nu, fnu) Compute the mean opacity to absorption for a given spectrum.

Methods (detail)

set_sublimation_temperature(mode, temperature=0.0)

Set the dust sublimation mode and temperature.

Parameters:
mode : str
The dust sublimation mode, which can be:
  • ‘no’ - no sublimation
  • ‘fast’ - remove all dust in cells exceeding the
    sublimation temperature
  • ‘slow’ - reduce the dust in cells exceeding the
    sublimation temperature
  • ‘cap’ - any temperature exceeding the sublimation
    temperature is reset to the sublimation temperature.
temperature : float, optional

The dust sublimation temperature, in K
set_sublimation_specific_energy(mode, specific_energy=0.0)

Set the dust sublimation mode and specific energy.

Parameters:
mode : str
The dust sublimation mode, which can be:
  • ‘no’ - no sublimation
  • ‘fast’ - remove all dust in cells exceeding the
    sublimation specific energy
  • ‘slow’ - reduce the dust in cells exceeding the
    sublimation specific energy
  • ‘cap’ - any specific energy exceeding the sublimation
    specific energy is reset to the sublimation specific energy.
specific_energy : float, optional

The dust sublimation specific energy, in cgs
set_lte_emissivities(n_temp=1200, temp_min=0.1, temp_max=100000.0)

Calculate the emissivities assuming LTE

Parameters:
n_temp : int, optional

The number of temperatures to calculate the emissivities for

temp_min : float, optional

The minimum temperature to calculate the emissivities for

temp_max : float, optional

The maximum temperature to calculate the emissivities for
plot(filename)
read(filename)

Read in from a standard dust file

write(filename, compression=True)

Write out to a standard dust file, including calculations of the mean opacities and optionally thermal emissivities.

temperature2specific_energy(temperature)

Convert a temperature to its corresponding specific energy value.

Parameters:
temperature : float or array_like

The temperature to convert
Returns:
specific_energy : float or array_like

The specific energy corresponding to the input temperature
specific_energy2temperature(specific_energy)

Convert a specific energy value to its corresponding temperature.

Parameters:
specific_energy : float or array_like

The specific energy to convert
Returns:
temperature : float or array_like

The temperature corresponding to the input specific energy
chi_nu_temperature(temperature)

Compute the mean opacity to extinction for a blackbody at a given temperature.

Parameters:
temperature : float

The temperature of the blackbody to use
Returns:
chi_nu_mean : float

The mean opacity to extinction
kappa_nu_temperature(temperature)

Compute the mean opacity to absorption for a blackbody at a given temperature.

Parameters:
temperature : float

The temperature of the blackbody to use
Returns:
kappa_nu_mean : float

The mean opacity to absorption
chi_nu_spectrum(nu, fnu)

Compute the mean opacity to extinction for a given spectrum.

Parameters:
nu : array_like

The frequencies, in Hz

fnu : array_like

The monochromatic fluxes per unit frequency. Units are unimportant since proportionality constants are cancelled out in the computation.
Returns:
chi_nu_mean : float

The mean opacity to extinction
kappa_nu_spectrum(nu, fnu)

Compute the mean opacity to absorption for a given spectrum.

Parameters:
nu : array_like

The frequencies, in Hz

fnu : array_like

The monochromatic fluxes per unit frequency. Units are unimportant since proportionality constants are cancelled out in the computation.
Returns:
kappa_nu_mean : float

The mean opacity to absorption