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Supernova remnants (SNRs) can be rich sources of information on the parent SNexplosion. Thus investigating the transition from the phase of SN to that ofSNR can be crucial to link these two phases of evolution. Here we aim to studythe early development of SNR in more details, paying the major attention to thetransition from the early-expansion stage to the Sedov stage and the roleplayed by magnetic field in this transition. To this end, sphericalmagneto-hydrodynamic simulations of SNRs have been performed to study theevolution of magnetic field in young SNRs and explore a sequence of the SNRevolutionary stages in the pre-radiative epoch. Remnants of three supernovatypes are considered, namely, SNIa, SNIc and SNIIP, that covers a wide space ofparameters relevant for SNRs. Changes in global characteristics and developmentof spatial distributions are analysed. It is shown that the radial component ofmagnetic field rapidly drops downstream of the forward shock. Therefore, theradially-aligned polarization patterns observed in few young SNRs cannot bereproduced in the one-dimensional MHD simulations. The period SNR takes for thetransition from the earliest ejecta-driven phase to the Sedov phase is longenough, with its distinctive physical features, headed by the energy conversionfrom mostly kinetic one to a fixed ratio between the thermal and kineticcomponents. This transition worth to be distinguished as a phase in SNRevolutionary scheme. The updated sequence of stages in SNR evolution could bethe free expansion (of gas) -- energy-conversion -- Sedov-Taylor --post-adiabatic -- radiative.

Magneto-hydrodynamic simulations of young supernova remnants and their energy-conversion phase