Jet simulations using Zeus-MP :
Collimated bipolar jets around young stars have been detected for decades.
The most plausible theory developed over the years states that
they are launched magneto-centrifugally from the sources (e.g., Blandford &
Payne 1982, Königl & Pudritz 2000).
High resolution spectra of T Tauri jets obtained by the Hubble Space Telescope (HST) during the past few years, especially those near the jet base (e.g., Ray et al. 2007, Coffey et al. 2007) and advancements in computer technology have made it possible to compare directly jet simulation results with observations. Of particular significance is the discovery of radial velocity shifts in several T Tauri jets (Coffey et al. 2004, 2007) that are indicative of jet rotation (Anderson et al. 2003). These observations reinforce the notion that the jets carry off the bulk of the angular momentum from the accretion disks around newly formed stars to allow the observed accretion to continue (Pudritz et al. 2007). Previous 3D time-dependent simulations of such jets (Ouyed et al. 2003) had only reached a few AU.
With the usage of SHARCNET, we have extended the simulations to a much larger scale, about 25 AU (~700 r_i; please see below), an unprecedented distance away from the source. It is also close to the physical scale that was probed by HST.
vinj = 0.008, rin=1.5r_i, at t = 817(end): v1, logd, B1
vinj = 0.004, r0=0.4, fr=0.1, logd at t = 1300:
at t = 1618 (end)
mu=-0.5 (Pelletier & Pudritz 92): vinj = 0.003, r0=0.5
logd at t = 1200 (new run)
logd at t = 1500
logd at t = 1600
logd at t = 1700
logd at t = 1800
logd at t = 2000
A 3D image Brian made at t = 1500
Some old ones: vinj= 0.005, rin=2r_i, at t = 885(end): v1, logd, B1 (i=50)
vinj= 0.005, rin=1.5ri, at t = 800: v1, logd, v2 (i=50)