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The detailed modelling of the spectra observed from the long GRB031203 hostgalaxy at different epochs during the 2003-2009 years is presented. The lineprofiles show FWHM of about 100 km/s. A broad line profile with FWHM < 400 km/sappears in the line sockets from the 2009 observations. We suggest that thenarrow lines show the velocity of star-burst (SB) debris, while the broad onesare due to the wind from SB stars. The spectra are emitted from the gasdownstream of different shock fronts which are at work on the edges of theemitting clouds. A head-on-back shock appears when the wind from the SB starsreaches the internal edge of the SB debris moving outwards. A head-on shock iscreated by collision of the debris with the ISM clouds.Line ratios in bothcases are calculated by the coupled effect of shock and photoionization fromthe SB. The models selected by fitting the calculated to the observed lineratios show that the ionization parameters, the shock velocities and the gaspre-shock densities slowly decrease with time.Oxygen metallicities(12+log(O/H)=8.3-8.48) are lower than solar (8.82) by a factor <3 and nitrogenmetallicities are lower than solar (12+log(N/H)=8.0) by factors of 3-5.

Shock fronts in the long GRB031203 host galaxy