A jupyter notebook for computing the X-ray photoabsorption cross sections from 0.1 keV to 100 keV. The code uses the atomic cross section analytic fits from Verner+1995 for photoionization and the Klein-Nishin formula for the Compton effect from Longair+2011.
This script uses numpy, matplotlib, scipy and ChiantiPy. ChiantiPy uses the data from the Chianti atomic database. Follow the instructions here to install this library.
The Verner+1995 data is in the associated .tsv file - this should not be touched! From the ViZieR data
The only other necessary file for the script to run is the abundance file (.abund). If this is changed, just change the line in the jupyter notebook and re-run. The abundance file needs, at least, all elements that will be used in the cross section calculation, although it can have more elements. All "#" characters will be skipped. Left column: element number. Middle column: element abbreviation. Right column: abundance, relative to solar, defined as log [X/H] = log10(eps_x) - 12 (see e.g., the Asplund+2009 review). The provided file comes from the Chianti database using the results of Lodders+2009
It produces several PDF plots of the cross sections to show the total and elemental contributions. It also produces a data file, xdr_xsecData.dat. This column has the format of Ntemp Nenergy (Temperature array) (Energy array) (Cross section data: Ntemp rows, Nenergy columns)
This file is read and stored in XrayCommonMain and must be in the runtime directory.
It also produces a file, for the selected temperature, of the cross section at a specified temperature (xsec_select.dat). This can be used for plotting purposes, etc.
Here is an example for a protosolar abundance:
