hyperion.dust.HenyeyGreensteinDust

class hyperion.dust.HenyeyGreensteinDust(nu, albedo, chi, g, p_lin_max)

This class should be used for dust properties that include scattering parameterized by the Henyey-Greenstein, 1941 function. The dust properties should be instatiated as:

d = HenyeyGreensteinDust(nu, albedo, chi, g, p_lin_max)

where nu, albedo, and chi are 1-D Numpy arrays containing the frequencies, albedo, and opacity to extinction respectively, and g and p_lin_max are also 1-D Numpy arrays containing the asymmetry parameter and the maximum linear polarization.

Method

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

Methods (detail)

set_sublimation_temperature(self, mode, temperature=0.0)

Set the dust sublimation mode and temperature.

Parameters

modestr

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.

temperaturefloat, optional

The dust sublimation temperature, in K

set_sublimation_specific_energy(self, mode, specific_energy=0.0)

Set the dust sublimation mode and specific energy.

Parameters

modestr

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_energyfloat, optional

The dust sublimation specific energy, in cgs

set_lte_emissivities(self, n_temp=1200, temp_min=0.1, temp_max=100000.0)

Calculate the emissivities assuming LTE

Parameters

n_tempint, optional

The number of temperatures to calculate the emissivities for

temp_minfloat, optional

The minimum temperature to calculate the emissivities for

temp_maxfloat, optional

The maximum temperature to calculate the emissivities for

plot(self, filename)

read(self, filename)

Read in from a standard dust file

write(self, filename, compression=True)

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

temperature2specific_energy(self, temperature)

Convert a temperature to its corresponding specific energy value.

Parameters

temperaturefloat or array_like

The temperature to convert

Returns

specific_energyfloat or array_like

The specific energy corresponding to the input temperature

specific_energy2temperature(self, specific_energy)

Convert a specific energy value to its corresponding temperature.

Parameters

specific_energyfloat or array_like

The specific energy to convert

Returns

temperaturefloat or array_like

The temperature corresponding to the input specific energy

chi_nu_temperature(self, temperature)

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

Parameters

temperaturefloat

The temperature of the blackbody to use

Returns

chi_nu_meanfloat

The mean opacity to extinction

kappa_nu_temperature(self, temperature)

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

Parameters

temperaturefloat

The temperature of the blackbody to use

Returns

kappa_nu_meanfloat

The mean opacity to absorption

chi_nu_spectrum(self, nu, fnu)

Compute the mean opacity to extinction for a given spectrum.

Parameters

nuarray_like

The frequencies, in Hz

fnuarray_like

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

Returns

chi_nu_meanfloat

The mean opacity to extinction

kappa_nu_spectrum(self, nu, fnu)

Compute the mean opacity to absorption for a given spectrum.

Parameters

nuarray_like

The frequencies, in Hz

fnuarray_like

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

Returns

kappa_nu_meanfloat

The mean opacity to absorption