photo module¶

Methods required for specifying the irradiance values at the top of the atmosphere as well as the photodissociation cross sections.

photo.blackbody_lambda(in_x, temperature)¶: Like blackbody_nu() but for \(B_{\lambda}(T)\).

photo.blackbody_nu(in_x, temperature)¶

Calculate blackbody flux per steradian, \(B_{\nu}(T)\).

Note

Use numpy.errstate to suppress Numpy warnings, if desired.

Warning

Output values might contain nan and inf.

Parameters

in_x : number, array-like, or ~astropy.units.Quantity: Frequency, wavelength, or wave number. If not a Quantity, it is assumed to be in Hz.
temperature : number, array-like, or ~astropy.units.Quantity: Blackbody temperature. If not a Quantity, it is assumed to be in Kelvin.

Returns

flux : ~astropy.units.Quantity: Blackbody monochromatic flux in \(erg \; cm^{-2} s^{-1} Hz^{-1} sr^{-1}\).

Raises

photo.getAverageSigmas(wave, sigmas)¶

Average the cross sections across the bins specified in settings.wavelengthHigh and settings.wavelengthLow

wave: input array specifying the bins to average to

sigmas: input array specifying the cross sections

photo.getBBspectrum()¶: Get blackbody irradiance based on parameters in input file.

photo.getIrradiance()¶: Wrapper function to pull irradiance data using method specified in input file

photo.getIrradianceData()¶: Get irradiance based on data in file specified in input file.

photo.getPhotoCrosssections()¶

Fill the settings.photocrosssections arrays with appropriate values.

Data taken from input/*crosssections.dat files from phidrates.space.swri.edu

photo.initIrradiance()¶: Integrate the irradiance to the bins specified in settings

photo.plotCrosssections(wave, sigma, species=None)¶: Plotting routine for quickly checking crosssections

photo.scaleIrradiance(irr)¶: Scales the irradiance based on the orbital distance.

photo.updateTemperature()¶: Update the temperature using the method specified in the input file.