2016ApJ...830..113G

Numerical simulations of the SVS 13 microjet and bow shock bubble are performed using the WENO method that reproduces the main features and dynamics of data from the Keck Telescope/OSIRIS velocity-resolved integral field spectrograph: an expanding, cooler bow shock bubble, with the bubble center moving at approximately 50 km s^–1 with a radial expansion velocity of 11 km s^–1, surrounding the fast, hotter jet, which is propagating at 156 km s^–1. Contact and bow shock waves are visible in the simulations both from the initial short jet pulse that creates the nearly spherical bow shock bubble and from the fast microjet, while a terminal Mach disk shock is visible near the tip of the continuous microjet, which reduces the velocity of the jet gas down to the flow velocity of the contact discontinuity at the leading edge of the jet. At 21.1 years 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 years, 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 µm [Fe ii] line-and the bow shock bubble-traced in the lower excitation 2.122 µm H₂ 1-0 S(1) line-projected onto the plane of the sky are presented, and are in good agreement with the Keck observations.