  Shock waves constitute discontinuities in matter which are relevant in
studying the plasma behaviour in astrophysical scenarios and in heavy-ion
collision. They can produce conical emission in relativistic collisions and are
also thought to be the mechanism behind the acceleration of energetic particles
in active galactic nuclei and gamma ray bursts. The shocks are mostly
hydrodynamic shocks. In a magnetic background they become magnetohydrodynamic
(MHD) shocks. For that reason we study the space-like and time-like shock
discontinuity in a magnetic plasma. The shocks induce a phase transition in the
plasma, here assuming a transition from hadron to quarks. The MHD conservation
conditions are derived across the shock. The conservation conditions are solved
for downstream velocities and flow angles for given upstream variables. The
shock conditions are solved at different baryon densities. For the space-like
shocks the anisotropy in the downstream velocity arises due to the magnetic
field. The downstream velocity vector always points downward with respect to
the shock normal. With the increase in density the anisotropy is somewhat
reduced. The magnetic field has effectively no effect on time-like shocks. The
slight anisotropy in the downstream flow velocities is caused by the boosting
that brings the quantities from the fluid frame to normal incidence (NI) frame.
