GGLINE
GGLINE model computes absorption of the gamma-rays by isotropic soft photons of a given energy. The transmitted flux is exponentially decreased F(E)=F_0(E) exp(-tau(E)). The parameters of the model are (1) the energy of the soft photon line, (2) “Thomson” optical depth tau_0= N_ph R sigma_T, where N_ph is the photon density, R is the characteristic size, and sigma_T is the Thomson cross-section, and (3) redshift of the source.
For details, see Poutanen J., Stern B.E., 2010, ApJ Letters, 717, L118.
The files are available in the dropbox.
COMPPS
COMPPS model computes Comptonization spectra is different geometries using exact numerical solution of the radiative transfer equation. The computational “iterative scattering method” is similar to the standard Lambda-iteration and is described in Poutanen J., Svensson R., 1996, ApJ, 470, 249 (PS96). This model has been incorporated to XSPEC 12 as a standard model.
BURSTATMO
Atmosphere model for X-ray bursting neutron star accounting for Compton scattering using relativistic kinetic equation and exact redistribution function.
If you use the model for the data analysis, please, refer to
Suleimanov V. et al. 2011, A&A, 527, A139
Suleimanov V. et al. 2012, A&A, 545, A120
Theoretical spectra of X-ray bursting neutron star (NS) model atmospheres are widely used for determination of the NS basic parameters such as their masses and radii. Compton scattering, that plays an important role in spectra formation at high luminosities, is often accounted for using the differential Kompaneets operator, while in other models a more general, integral operator for the Compton scattering kernel is used. We construct here accurate NS atmosphere models using exact treatment of Compton scattering with the integral relativistic kinetic equation and exact relativistic angle-dependent redistribution function.
Please, contact J. Poutanen for the files.