  Numerical simulations are performed using the WENO method of the SVS 13
micro-jet and bow shock bubble which reproduce the main features and dynamics
of Keck Telescope/OSIRIS velocity-resolved integral field spectrograph data: an
expanding cooler bow shock bubble, with the bubble center moving at
approximately 50 km/s with a radial expansion velocity of 11 km/s, surrounding
the fast hotter jet, which is propagating at 156 km/s. Contact and bow shock
waves are visible in the simulations from both the initial short jet pulse
which creates the nearly spherical bow shock bubble and from the fast
micro-jet, while a terminal Mach disk shock is visible near the tip of the
continuous micro-jet, which reduces the jet gas velocity down to the flow
velocity of the contact discontinuity at the leading edge of the jet. At 21.1
yr after the launch of the initial bubble pulse, the jet has caught up with and
penetrated almost all the way across the bow shock bubble of the slower initial
pulse. At times later than about 22 yr, the jet has penetrated through the
bubble and thereafter begins to subsume its spherical form. Emission maps from
the simulations of the jet---traced by the emission of the shock excited 1.644
micron [Fe II] line---and bow shock bubble---traced in the lower excitation
2.122 micron H_2 1--0 S(1) line---projected onto the plane of the sky are
presented, and are in good agreement with the Keck observations.
