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The coupling between time-dependent, multidimensional MHD numerical codes andradiative line emission is of utmost importance in the studies of the interplaybetween dynamical and radiative processes in many astrophysical environments,with particular interest for problems involving radiative shocks. There is awidespread consensus that line emitting knots observed in Herbig-Haro jets canbe interpreted as radiative shocks. In this paper we address two differentaspects relevant to the time-dependent calculations of the line intensityratios of forbidden transitions, resulting from the excitation by planar,time-dependent radiative shocks traveling in a stratified medium. The first oneconcerns the impact of the radiation and ionization processes included in thecooling model, and the second one the effects of the numerical grid resolution.In this paper we apply the AMR methodology to the treatment of radiating shocksand show how this method is able to vastly reduce the integration time. Thetechnique is applied to the knots of the HH 30 jet to obtain the observed lineintensity ratios and derive the physical parameters, such as density,temperature and ionization fraction. We consider the impact of two differentcooling functions and different grid resolutions on the results. We concludethat the use of different cooling routines has effects on results whose weightdepends upon the line ratio considered. Moreover, we find the minimum numericalresolution of the simulation grid behind the shock to achieve convergence inthe results. This is crucial for the forthcoming 2D calculations of radiativeshocks.

Time-dependent MHD shocks and line intensity ratios in the HH 30 jet: A focus on cooling function and numerical resolution