1994A&A...287..206D

We introduce realistic initial conditions for the ejecta density profile (power law) and propose to explain the silicon, sulphur and iron excess seen in Kepler's supernova remnant as associated with shocked enriched ejecta. We assume the composition of the interstellar medium to be solar. We describe the hydrodynamic interaction between the ejecta and the ambient medium with the self-similar solutions of Chevalier (1982). Using non-equilibrium ionization, we compute the synthetic spectrum and constrain it with the observations of the Solid State Spectrometer onboard the Einstein satellite, the Channel Multiplier Array and the Medium Energy counters onboard the Exosat satellite. Equipartition between the ions and the electrons is assumed. We modeled different types of supernovae (type Ia, type II, type Ib), modifying the ejecta composition, the supernova mass, the power law index of the stellar density profile and including or not pre-supernova mass loss. Models of a type II supernova, with mass of order of 10M_☉, without stellar wind are able to reproduce well the observed spectra including the iron lines.