  We present numerical simulations of the evolution of a supernova (SN) remnant
expanding into a uniform background medium with density $n_H = 1.0$ cm$^{-3}$
and temperature of $10^4$ K. We include a dynamically evolving non-equilibrium
ionisation (NEI) network (consisting of all the ions of H, He, C, N, O, Ne, Mg,
Si, S, Fe), frequency dependent radiation transfer (RT), thermal conduction,
and a simple dust evolution model, all intra-coupled to each other and to the
hydrodynamics. We assume spherical symmetry. Photo-ionisation, radiation
losses, photo-heating, charge-exchange heating/cooling and radiation pressure
are calculated on-the-fly depending on the local radiation field and ion
fractions. We find that the dynamics and energetics (but not the emission
spectra) of the SN remnants can be well modelled by collisional equilibrium
cooling curves even in the absence of non-equilibrium cooling and radiative
transport. We find that the effect of precursor ionising radiation at different
stages of SN remnant are dominated by rapid cooling of the shock and differ
from steady state shocks. The predicted column densities of different ions such
as N II, C IV and N V, can be higher by up to several orders of magnitude
compared to steady state shocks. We also present some high esolution emission
spectra that can be compared with the observed remnants to obtain important
information about the physical and chemical states of the remnant, as well as
constrain the background ISM.
