Jet simulations using <a 
href="http://www.astro.umd.edu/~vernaleo/zeusmp.html"> Zeus-MP </a>: 
<p>
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). <br>

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. <br>

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.  </p>

<p>
mu=-0.25 (BP82): <br>

<!-- vinj = 0.005 and r0=0.1, at t~427 (end)
<a href="v5t427.jpg">v2, logd and B2</a>
</p>
<p>
vinj= 0.007 and r0=0.1, at t = 430:

<a href="v7t430.jpg">v2, logd and B2</a>
<br>
at t = 557(end): <a href="v2logdB2t557.jpg">v2, logd and B2</a>
<img src="v2logdB2t557.jpg">
</p> -->
<p>
vinj = 0.008, rin=1.5r_i, at t = 817(end): v1, logd, B1
<img src="v1logdB1t817.jpg" height="" width=""> Sept. 2007
<br>
vinj = 0.004, r0=0.4, fr=0.1, logd at t = 1300: 
<img src="Jets/BPlogdt1300.jpg" height="" width=""> 
<br>
at t = 1618 (end)
<img src="Jets/BPlogdt1617.jpg" height="" width="">
</p>
<a 
href="http://www.capca.ucalgary.ca/~bniebergal/webPHP/research.php?subdir=jetsFromYSOs">
Brian's 3D images</a>
<hr>
vinj = 0.004, r0=0.5, fr=0.1 (new run): logd at t = 1300:
<img src="Jets/BPnlogdt1300.jpg" height="" width=""> <br>
logd at t = 1800
<img src="Jets/BPnlogdt1800.jpg"> 
<li> logd at z = 300 <img src="Jets/BPnlogdt18z300.jpg"> &nbsp;
logd at z = 550 <img src="Jets/BPnlogdt18z550.jpg"> </li>
v1 at t = 1800 <img src="Jets/BPv1zoomt1800.jpg">
v3 at t = 1800 <img src="Jets/BPnv3t1800.jpg">
<hr>
<p>
mu=-0.5 (Pelletier & Pudritz 92): vinj = 0.003, r0=0.5
<img src="Jets/PPlogdt1200.jpg" height="" width="">
logd at t = 1200 (new run)
<img src="Jets/PPlogdt1500.jpg" height="" width="">
logd at t = 1500
<img src="Jets/PPlogdt1600.jpg">
logd at t = 1600
<img src="Jets/PPlogdt1700.jpg">
logd at t = 1700
<img src="Jets/PPlogdt1800.jpg">
logd at t = 1800
<img src="Jets/PPlogdt2000.jpg" height="" width="">
logd at t = 2000
<br>
<img src="Jets/PP3D1.png"> A 3D image Brian made at t = 1500
</p><hr>
<p>
mu=-0.01: 
<a href="http://web.ics.purdue.edu/~jstaff/jets/april7/"> 
Jan's page</a><br>
Some old ones: 
vinj= 0.005, rin=2r_i, at t = 885(end): v1, logd, B1 (i=50)
<img src="v1logdB1t885.jpg" height="" width="">
</p>

<p>
vinj= 0.005, rin=1.5ri, at t = 800: v1, logd, v2 (i=50)
<img src="v1logdv2t800.jpg" height="" width="">
</p>