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Slow-mode shocks are important in understanding fast magnetic reconnection,jet formation and heating in the solar atmosphere, and other astrophysicalsystems. The atmospheric conditions in the solar chromosphere allow bothionised and neutral particles to exist and interact. Under such conditions,fine substructures exist within slow-mode shocks due to the decoupling andrecoupling of the plasma and neutral species. We study numerically the finesubstructure within slow-mode shocks in a partially ionised plasma, inparticular, analysing the formation of an intermediate transition within theslow-mode shock. High-resolution 1D numerical simulations are performed usingthe (P\underline{I}P) code using a two-fluid approach. We discover thatlong-lived intermediate (Alfven) shocks can form within the slow-mode shock,where there is a shock transition from above to below the Alfven speed and areversal of the magnetic field across the shock front. The collisional couplingprovides frictional heating to the neutral fluid, resulting in aSedov-Taylor-like expansion with overshoots in the neutral velocity and neutraldensity. The increase in density results in a decrease of the Alfven speed andwith this the plasma inflow is accelerated to above the Alfven speed within thefinite width of the shock leading to the intermediate transition. This processoccurs for a wide range of physical parameters and an intermediate shock ispresent for all investigated values of plasma-$\beta$, neutral fraction, andmagnetic angle. As time advances the magnitude of the magnetic field reversaldecreases since the neutral pressure cannot balance the Lorentz force. Theintermediate shock is long-lived enough to be considered a physical structure,independent of the initial conditions.

Intermediate shock substructures within a slow-mode shock occurring in partially ionised plasma