“…For dissipative models in simple geometries in the limit of vanishing dissipation, the intermediate shocks were shown not to be stable against certain perturbations. Traditionally ͑Akhiezer, Liubarski, and Polovin, 9 Germain, 10 Jeffrey and Taniuti 11 ͒, this failure of the test of evolutionarity was used to rule out the physical reality of intermediate shocks. However, after Wu 13 showed intermediate shocks to arise in numerical solutions of the dissipative MHD equations, a flurry of numerical and observational papers appeared on the structure and formation of intermediate shocks, [25][26][27][28][29] on their astrophysical implications, 30,31 on their relationship with magnetic reconnection, 32,33 on their significance for the Riemann problem, [34][35][36] on their occurrence in bow-shock flows, 37 and their possible breakup.…”