astrobear - Blog
https://bluehound.circ.rochester.edu/astrobear/blog
About blog postsen-USTrac 1.4.1Using AstroBEAR for Lab ExperimentsehansenTue, 19 Jul 2016 21:19:27 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen07192016
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen07192016<p>
AstroBEAR needs more physics in order to make it more applicable to lab experiments. I've been toying with this idea, and I don't think I'm going to get very far because it is quite complicated. However, I have been somewhat successful at hard-coding some 0th order approximations into a separate problem module (not usable by the rest of the code). Even the act of attempting to implement these things has forced me to learn about new physics, yay!
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<p>
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</p>
<h3 class="section" id="LaserDeposition">Laser Deposition</h3>
<p>
A simple dump of some fraction of laser energy onto a target surface (resonance absorption). Target heats up and the thermal pressure gradient launches a plume of plasma.
</p>
<p>
One of the tricky things here was the directional nature of the laser heating. Once the laser hits some critical density, it is only absorbed to a certain depth. Thus far, my code only works with single proc and a fixed grid.
</p>
<p>
A more clever implementation could make use of multiple processors and AMR. And to do laser deposition more accurately, you'd need ray tracing.
</p>
<p>
Now, the fun MHD stuff…
</p>
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</p>
<h3 class="section" id="BiermannBattery">Biermann Battery</h3>
<p>
In ideal MHD, we have the induction equation:
</p>
<p>
<span class="trac-mathjax" style="display:none">\frac{\partial \vec{B}}{\partial t} = \vec{\nabla} \times (\vec{v} \times \vec{B})</span>.
</p>
<p>
In resistive MHD, the induction equation becomes:
</p>
<p>
<span class="trac-mathjax" style="display:none">\frac{\partial \vec{B}}{\partial t} = \vec{\nabla} \times (\vec{v} \times \vec{B}) + \frac{\eta}{4\pi} \nabla^2 \vec{B}</span>
</p>
<p>
This is in some version of the code thanks to Shule. There are other MHD terms that can be important depending on the context of the problem. Here is the induction equation with the Biermann term:
</p>
<p>
<span class="trac-mathjax" style="display:none">\frac{\partial \vec{B}}{\partial t} = \vec{\nabla} \times (\vec{v} \times \vec{B}) + \frac{\eta}{4\pi} \nabla^2 \vec{B} + \frac{1}{e} \vec{\nabla} \times (\frac{\vec{\nabla} P}{n})</span>
</p>
<p>
The Biermann term makes self-generated B-fields possible. In other words, you don't need an initial B to generate more B. This is also in my new problem module, and could someday be implemented into AstroBEAR for general use. This formulation assumes the plasma is fully ionized (i.e. <span class="trac-mathjax" style="display:none">n = n_e</span>).
</p>
<p>
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</p>
<h3 class="section" id="NernstEffect">Nernst Effect</h3>
<p>
Lastly, we have the Nernst term. Here's how the induction equation becomes even more complicated:
</p>
<p>
<span class="trac-mathjax" style="display:none">\frac{\partial \vec{B}}{\partial t} = \vec{\nabla} \times ((\vec{v} + \vec{v_N}) \times \vec{B}) + \frac{\eta}{4\pi}\nabla^2 \vec{B} + \frac{1}{e} \vec{\nabla} \times (\frac{\vec{\nabla} P}{n})</span>
</p>
<p>
This <span class="trac-mathjax" style="display:none">\vec{v_N}</span> is the Nernst velocity, and it can be written as:
</p>
<p>
<span class="trac-mathjax" style="display:none">\vec{v_N} = \frac{\vec{q}}{2.5 P} = \frac{-\kappa \cdot \vec{\nabla} T}{2.5 P}</span>
</p>
<p>
where <span class="trac-mathjax" style="display:none">\vec{q}</span> is the heat flux and <span class="trac-mathjax" style="display:none">\kappa</span> is the thermal conductivity. <span class="trac-mathjax" style="display:none">\kappa</span> is technically a tensor since it is different in different directions (anisotropic). We can simplify the tensor and write <span class="trac-mathjax" style="display:none">\vec{q}</span> as follows:
</p>
<p>
<span class="trac-mathjax" style="display:none">\vec{q} = - \kappa_\parallel \vec{b}(\vec{\nabla}T \cdot \vec{b}) - \kappa_\perp \vec{b} \times (\vec{\nabla}T \times \vec{b}) -\kappa_\wedge (\vec{b} \times \vec{\nabla}T)</span>
</p>
<p>
where <span class="trac-mathjax" style="display:none">\vec{b}</span> is a unit vector in the direction of <span class="trac-mathjax" style="display:none">\vec{B}</span>. The first two terms are implemented somewhere in the code for conduction, but the third term is missing. Furthermore, I believe the conduction implementation in the code is strictly for transporting heat; in other words, there is no magnetic field generation.
</p>
<p>
This is something that I haven't implemented yet. There should be a way to add the Nernst velocity to the fluxes within the code, but I think I will first try to separate <span class="trac-mathjax" style="display:none">v_N</span> in the induction equation and treat it as a source term.
</p>
Mach Stems: Cooling Strength ==> Effective GammaehansenFri, 03 Jun 2016 17:15:27 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen06032016
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen06032016<p>
Below is a new set of 2-D runs designed to explore how the strength of radiative cooling affects Mach stem formation and size. An approximation of the critical angle for Mach stem formation depends only on the adiabatic index gamma. We hypothesize that the cooling strength implies an "effective" gamma such that very weak cooling implies a gamma of 5/3 and very strong cooling implies a gamma of 1.
</p>
<p>
Furthermore, if a Mach stem forms, its size is limited to the smaller of the cooling length and the clump diameter. Thus, as cooling strength increases (decreasing cooling length), the size of the Mach stem should decrease.
</p>
<p>
Here are the important parameters:
</p>
<pre class="wiki">vs = 50 km/s
M = 5.2
T = 8322.56 K
nclump/namb = 5000
tfinal = 100 yrs
Rclump = 10 AU
</pre><table class="wiki">
<tr><th> dcool / Rclump </th><th> Ambient Density [cm<sup>-3</sup>] </th><th> d / Rclump </th><th> Cooling Run </th><th> Effective Gamma Run
</th></tr><tr><th> 30 </th><th> 3.18 </th><th> 5 </th><th> <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen06032016/M5.2_dcool300.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen06032016/M5.2_dcool300.png" width="200" /></a> </th><th> 1.46 <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen06032016/M5.2_dcool300_g1.46.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen06032016/M5.2_dcool300_g1.46.png" width="200" /></a>
</th></tr><tr><th> 10 </th><th> 9.77 </th><th> 4 </th><th> <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen06032016/M5.2_dcool100.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen06032016/M5.2_dcool100.png" width="200" /></a> </th><th> 1.25 <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen06032016/M5.2_dcool100_g1.25.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen06032016/M5.2_dcool100_g1.25.png" width="200" /></a>
</th></tr><tr><th> 3 </th><th> 33.95 </th><th> 3 </th><th> <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen06032016/M5.2_dcool30.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen06032016/M5.2_dcool30.png" width="200" /></a> </th><th> 1.19 <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen06032016/M5.2_dcool30_g1.19.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen06032016/M5.2_dcool30_g1.19.png" width="200" /></a>
</th></tr><tr><th> 1 </th><th> 108.21 </th><th> 2.4 </th><th> <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen06032016/M5.2_dcool10.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen06032016/M5.2_dcool10.png" width="200" /></a> </th><th> 1.14 <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen06032016/M5.2_dcool10_g1.14.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen06032016/M5.2_dcool10_g1.14.png" width="200" /></a>
</th></tr><tr><th> 0.3 </th><th> 388.55 </th><th> unstable </th><th> <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen06032016/M5.2_dcool3.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen06032016/M5.2_dcool3.png" width="200" /></a> </th><th> ⇐ 1.10 <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen06032016/M5.2_dcool3_g1.10.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen06032016/M5.2_dcool3_g1.10.png" width="200" /></a>
</th></tr><tr><th> 0.1 </th><th> 1252.4 </th><th> unstable </th><th> </th><th> ⇐ 1.10
</th></tr></table>
<p>
Then, there are 5 more runs with M = 30 and T = 250.047 K.
</p>
<table class="wiki">
<tr><th> dcool / Rclump </th><th> Ambient Density [cm<sup>-3</sup>] </th><th> d / Rclump </th><th> Cooling Run </th><th> Effective Gamma Run
</th></tr><tr><th> 30 </th><th> 3.634 </th><th> 5 </th><th> <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen06032016/M30_dcool300.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen06032016/M30_dcool300.png" width="200" /></a> </th><th> 1.50 <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen06032016/M30_dcool300_g1.50.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen06032016/M30_dcool300_g1.50.png" width="200" /></a>
</th></tr><tr><th> 10 </th><th> 11.16 </th><th> 4 </th><th> <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen06032016/M30_dcool100.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen06032016/M30_dcool100.png" width="200" /></a> </th><th> 1.30 <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen06032016/M30_dcool100_g1.30.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen06032016/M30_dcool100_g1.30.png" width="200" /></a>
</th></tr><tr><th> 3 </th><th> 38.76 </th><th> 3 </th><th> <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen06032016/M30_dcool30.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen06032016/M30_dcool30.png" width="200" /></a> </th><th> 1.18 <img alt="No image "M30_dcool30_g1.18.png" attached to Blog: Mach Stems: Cooling Strength ==> Effective Gamma" src="/astrobear/chrome/common/attachment.png" title="No image "M30_dcool30_g1.18.png" attached to Blog: Mach Stems: Cooling Strength ==> Effective Gamma" width="200" />
</th></tr><tr><th> 1 </th><th> 123.30 </th><th> unstable </th><th> <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen06032016/M30_dcool10.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen06032016/M30_dcool10.png" width="200" /></a> </th><th style="text-align: right"> ⇐ 1.10 <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen06032016/M30_dcool10_g1.10.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen06032016/M30_dcool10_g1.10.png" width="200" /></a>
</th></tr></table>
<p>
The effect of cooling is stronger than I had anticipated, and I'm not sure if we can use Pat's figure from his recent Mach stem paper to make quantitative comparisons. However, qualitatively, we are already proving our point, and more simulations with lowered gamma instead of cooling can lead to values for effective gamma.
</p>
Meeting Update 05/11/2016 - EddieehansenWed, 11 May 2016 16:16:58 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen05112016
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen05112016<ul><li>Finished thesis last week! woohoo!
</li></ul><ul><li>Clumpy paper and response to referee is written. Ready to resubmit?
</li></ul><ul><li>Cooling paper is written. Need more details on other codes. Pat will add some writing in 1-D radiative shocks section?
</li></ul><ul><li>Resumed 3-D pulsed jet sims. Hydro and beta = 1 runs are done. beta = 5 is 95% done, beta = 0.4 is 66% done and may take a few more weeks to finish on bluehive. Maybe only 2 weeks if I can get a reservation for more nodes?
</li></ul><ul><li>Finished poster for next week's HEDLA conference:
</li></ul><p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen05112016/Hansen_HEDLA16_poster.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen05112016/Hansen_HEDLA16_poster.png" width="300" /></a>
</p>
More 2-D Mach stem runs w/ coolingehansenWed, 20 Apr 2016 14:51:12 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen04202016
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen04202016<p>
Previous blog posts: <a href="https://bluehound.circ.rochester.edu/astrobear/blog/ehansen04122016">ehansen04122016</a>, <a href="https://bluehound.circ.rochester.edu/astrobear/blog/ehansen04192016">ehansen04192016</a>
</p>
<p>
Did a few runs with d/Rclump = 6 where the previous runs were closer together at d/Rclump = 4.
</p>
<table class="wiki">
<tr><th> Rclump/Lcool </th><th> At 50 years </th><th> Mach stem size
</th></tr><tr><th> 2 </th><th> <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen04202016/2Lcool_d6.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen04202016/2Lcool_d6.png" width="300" /></a> </th><th> regular reflection
</th></tr><tr><th> 1 </th><th> <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen04202016/1Lcool_d6.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen04202016/1Lcool_d6.png" width="300" /></a> </th><th> 0.3 Lcool
</th></tr><tr><th> 0.5 </th><th> <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen04202016/0.5Lcool_d6.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen04202016/0.5Lcool_d6.png" width="300" /></a> </th><th> 0.4 Lcool
</th></tr></table>
<p>
Also did a run where we are no longer in the frame of reference of the clump and shock; both ambient and clump are moving now, but relative velocity is the same as before. With d/Rclump = 4 and Lcool = 0.05 Rclump. It looked the same, i.e. no instability.
</p>
Meeting Update 04/19/2016 - EddieehansenTue, 19 Apr 2016 17:13:53 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen04192016
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen04192016<ul><li>Updated table on Mach stems and Lcool: <a href="https://bluehound.circ.rochester.edu/astrobear/blog/ehansen04122016">ehansen04122016</a>
<ul><li>Checked to see if low resolution is cause of bow shock instability: doesn't appear to be, image below
</li><li>Checked if 3-D effects cause bow shock instability: plausible, image below
</li><li>Checked if even stronger cooling (Lcool = Rclump / 100) is the cause: also plausible, movie below.
</li><li>My thoughts: any small perturbation can trigger the instability whether it be numerical or physical. The stronger the cooling, the easier it is to perturb. I believe my simulations in the clumpy paper are more susceptible simply because they are 3-D; extra degree of freedom for motions and/or noise. Also, in the paper, we are not in the frame of reference of the fast clump.
</li></ul></li></ul><p>
Lcool = 0.1 Rclump, 2-D, low res <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen04192016/2D_10Lcool_lowres.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen04192016/2D_10Lcool_lowres.png" width="300" /></a>
</p>
<p>
Lcool = 0.1 Rclump, 3-D slice <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen04192016/3D_10Lcool.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen04192016/3D_10Lcool.png" width="300" /></a>
</p>
<p>
2-D, nice Mach stem, <a class="attachment" href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen04192016/2Lcool.gif" title="Attachment '2Lcool.gif' in Blog: Meeting Update 04/19/2016 - Eddie">Lcool = 0.5 Rclump movie</a><a class="trac-rawlink" href="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen04192016/2Lcool.gif" title="Download"></a>
</p>
<p>
2-D, unstable?, <a class="attachment" href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen04192016/100Lcool.gif" title="Attachment '100Lcool.gif' in Blog: Meeting Update 04/19/2016 - Eddie">Lcool = 0.01 Rclump movie</a><a class="trac-rawlink" href="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen04192016/100Lcool.gif" title="Download"></a>
</p>
<p>
<br />
</p>
<ul><li>I should be able to finish up referee report and resubmit clumpy paper by end of week.
</li></ul><ul><li>Pat is working on cooling paper, and I will add some more details this week.
</li></ul><ul><li>Thesis is coming along nicely. Most of the writing is finished except for the conclusions section.
</li></ul>Meeting Update 04/12/2016 - EddieehansenTue, 12 Apr 2016 15:34:20 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen04122016
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen04122016<ul><li>HEDLA XI accepted my abstract, gave me a poster presentation
</li></ul><ul><li>While writing up the introduction for my thesis, I decided it would be nice to have a schematic of a disk-jet system so I drew one.
</li></ul><p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen04122016/disk-jet.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen04122016/disk-jet.png" width="300" /></a>
</p>
<ul><li>In response to referee report on the 3-D clumpy paper, I am running some 2-D sims to look at Mach stem size when cooling is present. For each simulation, I change Rclump to see if Mach stem size is limited by Lcool !and/or Rclump.
</li></ul><p>
All runs have M = 7 and Lcool = 12.7 AU.
</p>
<p>
1 computational unit = 1 Lcool.
</p>
<p>
separation distance d = 4 Rclump
</p>
<table class="wiki">
<tr><th> Rclump/Lcool </th><th> At 50 years </th><th> Mach stem size
</th></tr><tr><th> 100 </th><th> <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen04122016/100Lcool.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen04122016/100Lcool.png" width="300" /></a> </th><th> regular reflection, unstable?
</th></tr><tr><th> 20 </th><th> <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen04122016/20Lcool.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen04122016/20Lcool.png" width="300" /></a> </th><th> regular reflection
</th></tr><tr><th> 10 </th><th> <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen04122016/10Lcool.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen04122016/10Lcool.png" width="300" /></a> </th><th> regular reflection
</th></tr><tr><th> 2 </th><th> <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen04122016/2Lcool.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen04122016/2Lcool.png" width="300" /></a> </th><th> approximately 0.5 Lcool
</th></tr><tr><th> 1 </th><th> <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen04122016/1Lcool.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen04122016/1Lcool.png" width="300" /></a> </th><th> approximately 1 Lcool
</th></tr><tr><th> 0.5 </th><th> <a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen04122016/0.5Lcool.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen04122016/0.5Lcool.png" width="300" /></a> </th><th> forming single bow
</th></tr></table>
<p>
So it does appear that when cooling is strong (Rclump/Lcool ≥ 1), the Mach stem size is limited by Lcool or it's even smaller. However, I'm not convinced that when cooling is weak, the Mach stem size will be limited by Rclump.
</p>
Update 03/28/16 - EddieehansenMon, 28 Mar 2016 15:51:41 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen03282016
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen03282016<ul><li>3-D pulsed jets are still running, only hydro run is finished. Beta = 1 run will be done in about a week on bluehive, beta = 5 is 75% done and beta = 0.4 is only 50% done on davinci. The queues on davinci take way too long, so I'm going to move the beta = 0.4 run to bluehive as well. It'll take a while since I can only get 120 cores, but at least it'll be making progress.
</li></ul><p>
<a class="attachment" href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen03282016/hydro_emiss.gif" title="Attachment 'hydro_emiss.gif' in Blog: Update 03/28/16 - Eddie">hydro emission movie</a><a class="trac-rawlink" href="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen03282016/hydro_emiss.gif" title="Download"></a>
</p>
<ul><li>Ready to finish response to referee report on clumpy paper. Need to have meeting with Pat.
</li></ul><ul><li>Finished first draft of cooling paper, ready to revise and add figures. Working on some cooling curve plots now.
</li></ul>Update 03/11/2016 - EddieehansenFri, 11 Mar 2016 17:35:58 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen03112016
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen03112016<ul><li>Worked on cooling paper: abstract, intro, methods sections finished. Might've finished the whole thing had I not focused so much on recent referee report. I can release these sections for edits, and continue working on the rest.
</li></ul><ul><li>Worked on referee report for clumpy paper. I think most of it is resolved, and I don't think we have to change the paper too much. However, we still need to have a co-author discussion about gammas, cooling, and Mach stems. Below is a test simulation I ran to show that simulating a more "realistic" clump does not change our conclusions.
</li></ul><p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen03112016/realclump_7.5yrs.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen03112016/realclump_7.5yrs.png" width="300" /></a>
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen03112016/realclump_32yrs.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen03112016/realclump_32yrs.png" width="300" /></a>
</p>
<ul><li>3-D jet simulations are still going. Here's a status update:
</li></ul><table class="wiki">
<tr><th> Beta </th><th> Frame (out of 120) </th><th> Est. Wall Time Remaining
</th></tr><tr><th> Inf </th><th> 103 </th><th> 10.7 hours
</th></tr><tr><th> 5 </th><th> 76 </th><th> 2.1 days
</th></tr><tr><th> 1 </th><th> 88 </th><th> 17.4 days
</th></tr><tr><th> 0.4 </th><th> 55 </th><th> 4.2 days
</th></tr></table>
<p>
The beta=1 run will take significantly longer because it's on bluehive, but the other runs wait in the queue for so long in between restarts on davinci that all of these runs may finish around the same time in 3 weeks or so. Honestly don't see this project finishing in time to be part of my thesis, especially since we wanted to do additional runs with random pulses, less frequent pulses, no pulses, etc.
</p>
Update 02/18/16 - EddieehansenThu, 18 Feb 2016 19:32:14 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen02182016
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen02182016<ul><li>Monday, I was busy gathering/generating some old data for Pat for the Mach stem paper. Revisions according to referee report should have been submitted yesterday.
</li></ul><ul><li>Been putting my thesis together and writing the cooling paper which will also be a chapter in my thesis.
</li></ul><ul><li>Running the 3-D pulsed jets on davinci. Might move to bluehive since the queue on davinci is taking forever. Below is the beta = 1 run. I changed the scaling on the emission to make it brighter. It doesn't look like there is enough resolution to separate the H-alpha and [S II] lines within a clump, but we do see H-alpha (green) leading the clumps (yellow).
</li></ul><p>
<a class="attachment" href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen02182016/mhd1coldensemiss.gif" title="Attachment 'mhd1coldensemiss.gif' in Blog: Update 02/18/16 - Eddie">MHD1 movie</a><a class="trac-rawlink" href="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen02182016/mhd1coldensemiss.gif" title="Download"></a>
</p>
Update 02/08/16 - EddieehansenMon, 08 Feb 2016 14:41:20 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen02082016
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen02082016<ul><li>Clumpy paper is done. Time to submit?
</li></ul><ul><li>Writing cooling paper, and thesis.
</li></ul><ul><li>Running 3-D jet sims. The only thing I don't like so far is that the magnetized runs seem to have pressure (probably magnetic pressure) pushing radially outwards at the injection region. See images and movies below…
</li></ul><p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen02082016/2jetsrhoslice.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen02082016/2jetsrhoslice.png" width="300" /></a>
</p>
<p>
<a class="attachment" href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen02082016/2jetsrhoslice.gif" title="Attachment '2jetsrhoslice.gif' in Blog: Update 02/08/16 - Eddie">movie</a><a class="trac-rawlink" href="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen02082016/2jetsrhoslice.gif" title="Download"></a>
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen02082016/2jetscoldens.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen02082016/2jetscoldens.png" width="300" /></a>
</p>
<p>
<a class="attachment" href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen02082016/2jetscoldens.gif" title="Attachment '2jetscoldens.gif' in Blog: Update 02/08/16 - Eddie">movie</a><a class="trac-rawlink" href="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen02082016/2jetscoldens.gif" title="Download"></a>
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen02082016/2jetsemiss.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen02082016/2jetsemiss.png" width="300" /></a>
</p>
<p>
<a class="attachment" href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen02082016/2jetsemiss.gif" title="Attachment '2jetsemiss.gif' in Blog: Update 02/08/16 - Eddie">movie</a><a class="trac-rawlink" href="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen02082016/2jetsemiss.gif" title="Download"></a>
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen02082016/hydrocoldensemiss.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen02082016/hydrocoldensemiss.png" width="300" /></a>
</p>
<p>
<a class="attachment" href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen02082016/hydrocoldensemiss.gif" title="Attachment 'hydrocoldensemiss.gif' in Blog: Update 02/08/16 - Eddie">movie</a><a class="trac-rawlink" href="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen02082016/hydrocoldensemiss.gif" title="Download"></a>
</p>
Update 01/25/16 - EddieehansenMon, 25 Jan 2016 16:29:15 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen01252016
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen01252016<p>
Nothing new to post in terms of images or movies, so here's an update on what I'm currently working on:
</p>
<ul><li>Clumpy paper: Received another round of comments from Pat. Time to discuss these and figure out how best to edit the paper.
</li></ul><ul><li>Cooling paper: Writing up the Methods section which includes a bunch of new equations that I haven't included in any of my other papers. I'm giving myself an arbitrary deadline to have a completed first draft by the end of February.
</li></ul><ul><li>3-D jet simulations: These are running on Rice's Davinci. Looks like it takes about 1 week per run (not including wait times).
</li></ul><ul><li>Thesis: Started putting this together. Not much writing done yet, but I have a formatted template now.
</li></ul><ul><li>Job search: I'm going to give a talk at the LLE on Wednesday Feb. 9th. Still need to decide which of my projects I want to present. Also, need to schedule an interview with Paul Drake's group (U. Mich.)
</li></ul><p>
I think that's everything. I'm pretty busy these days…
</p>
Update 01/11/16 - EddieehansenMon, 11 Jan 2016 17:39:29 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen01112016
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen01112016<ul><li>Finished another round of edits for 3-D clumpy paper
</li></ul><ul><li>Got the 3-D pulsed jets running faster now.
<ul><li>On 576 cores, I got the MHD run w/ beta = 1 to run 94 out of 120 frames in just 8 hours.
</li><li>This was at a lower resolution of 32 cells per jet radius, and the jet propagated to a distance of about 23 jet radii.
</li><li>I suspect this run would take about 6 more hours to get the full 120 frames. Meaning that a run at the desired 64 cells per jet radius should take a little over one week to finish. This is doable.
</li></ul></li></ul><p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen01112016/MHD1_rho.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen01112016/MHD1_rho.png" width="300" /></a>
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen01112016/MHD1_emiss.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen01112016/MHD1_emiss.png" width="300" /></a>
</p>
<p>
Still having issues with Visit on Grass. I hope Rich can fix the issue soon, so that I can make movies more easily.
</p>
Update 11/30/2015 - EddieehansenMon, 30 Nov 2015 17:48:28 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen11302015
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen11302015<ul><li>I've applied to several jobs now, but need to do more.
</li></ul><ul><li>Working on rewrites for paper. Plan on finishing it by the end of this week.
</li></ul><ul><li>MHD version of 3D pulsed jets was having some restart issues, but I fixed it. Below is an image from a run with an initially purely toroidal field with beta = 1, with 64 cells per jet radius. This run (6 out of 120 frames) took 3 hours on 576 cores. The current standard output estimates that the run will take about 3 weeks to finish. Perhaps it's a better idea to do a longer run at a lower resolution (32 cells per jet radius) before continuing with this production-level run. I just don't want to waste time and resources if there turns out to be some difficult-to-explain-weirdness in the jet at later times.
</li></ul><p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen11302015/MHD1_tor.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen11302015/MHD1_tor.png" width="300" /></a>
</p>
Update 11/16/2015 - EddieehansenMon, 16 Nov 2015 18:11:49 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen11162015
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen11162015<ul><li>working on edits for 3D bow shock interactions paper
</li></ul><ul><li>applying to jobs
</li></ul><ul><li>still trying to figure out waviness in 3D precessing jets
<ul><li>Things I have tried so far:
<ul><li>primitive limiters instead of characteristic
</li><li>lower CFL
</li><li>outflow object inside lower z boundary
</li><li>velocity fade in radial direction
</li><li>no pulses
</li><li>H viscosity
</li><li>apply diffusion
</li><li>smaller precession angle
</li></ul></li><li>Noticed some potentially odd things:
<ul><li>jet boundary looks tilted in first frame, likely due to precession in magnitude of the velocity in z-directio
</li><li>the magnitudes of the velocity in every direction x, y, z seem to be precessing. I don't think this is what we want. I think vz should be constant in time (except for the pulsations of course), and vx and vy should change but in a way such that at any given time they are constant throughout the outflow object. In the current implementation, there appears to be a phi dependence on magnitude.
</li></ul></li></ul></li></ul><p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen11162015/tilt.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen11162015/tilt.png" width="200" /></a>
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen11162015/vx.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen11162015/vx.png" width="200" /></a>
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen11162015/vz.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen11162015/vz.png" width="200" /></a>
</p>
Update 11/09/2015 - EddieehansenMon, 09 Nov 2015 17:22:27 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen11092015
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen11092015<ul><li>Made image from HH 2 for my 3D clumpy paper. This is to compare with the multi-clump simulation since both show a shock "sheet".
</li></ul><p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen11092015/HH2_e2.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen11092015/HH2_e2.png" width="200" /></a>
</p>
<ul><li>We wanted to do another comparison figure with HH 34 to show lateral motion, but this is looking a bit trickier than I thought it would be because the .fits images are not aligned with each other. Waiting to hear back from Pat to see if there is an easy way to deal with this.
</li></ul><ul><li>Having issues with Grass and with my account on the Rice machine, so I don't have all of the data from some of my new 3D pulsed jet runs. Below are images from a 0 deg precession and a 1 deg precession run. I have simulation data for a run with increased refinement around the outflow object, and a run where the outflow object is inside the bottom domain boundary; I just can't get to the data right now. Below is an image comparing runs with 0, 1, and 3 deg precession from left to right respectively.
</li></ul><p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen11092015/PrecComp.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen11092015/PrecComp.png" width="200" /></a>
</p>
<ul><li>Lastly, I worked on my CV and I've been busy for the past few days applying for some national lab jobs.
</li></ul>Update 11/02/2015 - EddieehansenMon, 02 Nov 2015 16:51:44 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen11022015
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen11022015<p>
Using ds9 and gimp to generate a couple of figures for my 3D clumpy paper that will show an HST image and a simulation image side-by-side. Below is an example:
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen11022015/HH1compfig.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen11022015/HH1compfig.png" width="300" /></a>
</p>
<p>
<br />
</p>
<h3 class="section" id="a3DJets">3D Jets</h3>
<p>
I've tried several things, and I still see the waves in all cases:
</p>
<ul><li>For some reason, the exact Riemann solver does not work well. Code stops early due to nan in flux.
</li><li>Added velocity fade from 0 to Rjet. This is not a precession fade, just a velocity magnitude fade.
</li><li>Turned off characteristic limiters, use primitive limiters instead.
</li><li>Turned on <a class="missing wiki">ApplyDiffusion</a>.
</li><li>Lowered target CFL from 0.3 to 0.1.
</li><li>Turned off pulsations.
</li></ul><p>
Below is an image from the run with no pulses:
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen11022015/hydro_nopulses.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen11022015/hydro_nopulses.png" width="300" /></a>
</p>
Update 10/19/2015 - EddieehansenMon, 19 Oct 2015 15:42:43 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen10192015
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen10192015<p>
Below is image/movie showing the hydro 3-D pulsed jet: slice of x-z plane, slice of y-z plane, and column density.
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen10192015/hydro_slices.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen10192015/hydro_slices.png" width="300" /></a>
</p>
<p>
<a class="attachment" href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen10192015/hydro_slices.gif" title="Attachment 'hydro_slices.gif' in Blog: Update 10/19/2015 - Eddie">movie</a><a class="trac-rawlink" href="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen10192015/hydro_slices.gif" title="Download"></a>
</p>
<p>
It might be helpful to review how the outflow object is set up: <a class="wiki" href="https://bluehound.circ.rochester.edu/astrobear/wiki/OutflowObjects">OutflowObjects</a>
</p>
<p>
My jet uses a radius = Rjet/2, thickness = Rjet/4, base = Rjet, and open_angle = 0. The outflow object steps on some cells, but the rest of the lower boundary is extrapolated; should probably change this to reflecting.
</p>
<p>
<br />
</p>
<h3 class="section" id="ThingsToTry">Things To Try</h3>
<ul><li>use different Riemann solver
</li><li>adjust CFL
</li><li>adjust boundary conditions of outflow object (radius, thickness, <strong>fade</strong>, etc.)
</li><li>turn off pulsations
</li><li>have precession fade from 0 to Rjet
</li></ul><p>
<br />
</p>
<h3 class="section" id="UPDATE">UPDATE</h3>
<p>
Things i have tried thus far:
</p>
<ul><li>For some reason, the exact Riemann solver does not work well. Code stops early due to nan in flux.
</li><li>Added velocity fade from 0 to Rjet. This is not a precession fade, just a velocity magnitude fade. Still see waves.
</li><li>Turned off characteristic limiters, use primitive limiters instead. Still see waves.
</li><li>Turned on ApplyDiffusion.
</li><li>Lowered target CFL from 0.3 to 0.1.
</li><li>Turned off pulsations.
</li></ul>Update 10/13/2015 - EddieehansenTue, 13 Oct 2015 18:01:30 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen10132015
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen10132015<h3 class="section" id="a2DMachstemresultswithlowM">2D Mach stem results with low M</h3>
<p>
low M = 1.55
</p>
<p>
TMS, SB = Transient Mach Stem, develops into a Single Bow shock
</p>
<p>
SMS = Stable Mach Stem
</p>
<p>
RR = Regular Reflection
</p>
<table class="wiki">
<tr><th> <strong>gamma</strong> </th><th> <strong>d</strong> </th><th> <strong>Result</strong>
</th></tr><tr><th> 5/3 </th><th> 24 </th><th> RR
</th></tr><tr><th> 5/3 </th><th> 23 </th><th> SMS
</th></tr><tr><th> 5/3 </th><th> 22 </th><th> SMS
</th></tr><tr><th> 5/3 </th><th> 21 </th><th> SMS
</th></tr><tr><th> 5/3 </th><th> 18 </th><th> SMS
</th></tr><tr><th> 5/3 </th><th> 12 </th><th> SMS
</th></tr><tr><th> 5/3 </th><th> 11 </th><th> SMS
</th></tr><tr><th> 5/3 </th><th> 10 </th><th> SMS
</th></tr><tr><th> 5/3 </th><th> 9 </th><th> TMS, SB
</th></tr><tr><th> </th><th> </th><th>
</th></tr><tr><th> </th><th> </th><th>
</th></tr><tr><th> 1.4 </th><th> 21 </th><th> RR
</th></tr><tr><th> 1.4 </th><th> 20 </th><th> SMS
</th></tr><tr><th> 1.4 </th><th> 19 </th><th> SMS
</th></tr><tr><th> 1.4 </th><th> 18 </th><th> SMS
</th></tr><tr><th> 1.4 </th><th> 17 </th><th> SMS
</th></tr><tr><th> 1.4 </th><th> 15 </th><th> SMS
</th></tr><tr><th> 1.4 </th><th> 12 </th><th> SMS
</th></tr><tr><th> 1.4 </th><th> 11 </th><th> SMS
</th></tr><tr><th> 1.4 </th><th> 10 </th><th> SMS
</th></tr><tr><th> 1.4 </th><th> 9 </th><th> SMS
</th></tr><tr><th> 1.4 </th><th> 8 </th><th> TMS, SB
</th></tr><tr><th> 1.4 </th><th> 6.5 </th><th> TMS, SB
</th></tr><tr><th> 1.4 </th><th> 6 </th><th> TMS, SB
</th></tr><tr><th> 1.4 </th><th> 5 </th><th> TMS, SB
</th></tr><tr><th> 1.4 </th><th> 4.5 </th><th> TMS, SB
</th></tr><tr><th> </th><th> </th><th>
</th></tr><tr><th> </th><th> </th><th>
</th></tr><tr><th> 1,2 </th><th> 18 </th><th> RR
</th></tr><tr><th> 1,2 </th><th> 17 </th><th> SMS
</th></tr><tr><th> 1,2 </th><th> 16 </th><th> SMS
</th></tr><tr><th> 1,2 </th><th> 15 </th><th> SMS
</th></tr><tr><th> 1,2 </th><th> 13 </th><th> SMS
</th></tr><tr><th> 1.2 </th><th> 12 </th><th> SMS
</th></tr><tr><th> 1.2 </th><th> 9 </th><th> SMS
</th></tr><tr><th> 1.2 </th><th> 8 </th><th> SMS
</th></tr><tr><th> 1.2 </th><th> 7 </th><th> TMS, SB
</th></tr><tr><th> 1.2 </th><th> 6 </th><th> TMS, SB
</th></tr><tr><th> 1.2 </th><th> 5 </th><th> TMS, SB
</th></tr><tr><th> 1.2 </th><th> 4 </th><th> TMS, SB
</th></tr></table>
<p>
<br />
</p>
<h3 class="section" id="a3DPulsedJets">3D Pulsed Jets</h3>
<p>
Ran the MHD, beta = 1 model farther at 32 cells/Rjet.
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen10132015/MHD_1_rho.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen10132015/MHD_1_rho.png" width="300" /></a>
</p>
<p>
<a class="missing attachment">movie</a>
</p>
<p>
Started a production-quality hydro run at 64 cells/Rjet.
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen10132015/hydro_rho.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen10132015/hydro_rho.png" width="300" /></a>
</p>
<p>
<a class="attachment" href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen10132015/hydro_rho.gif" title="Attachment 'hydro_rho.gif' in Blog: Update 10/13/2015 - Eddie">movie</a><a class="trac-rawlink" href="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen10132015/hydro_rho.gif" title="Download"></a>
</p>
<p>
<br />
</p>
<h3 class="section" id="a3DClumpBowInteractionPaper">3D Clump/Bow Interaction Paper</h3>
<ul><li>Having some trouble with ds9 and the .fits images. I just want images that look like the ones from Pat's 2011 paper, but I can't seem to get the scaling quite right.
</li></ul>2D Mach stem results for low M, gamma = 1.4ehansenThu, 01 Oct 2015 19:15:09 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen10012015
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen10012015<p>
M = 1.55, gamma = 1.4
</p>
<p>
d = 8, 9, 10, 11, 12
</p>
<p>
All appear to show a Mach stem at the end of the simulation (triple points still visible) except for d = 8 which forms a single bow.
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen10012015/g1.4_M1.55_d8.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen10012015/g1.4_M1.55_d8.png" width="200" /></a>
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen10012015/g1.4_M1.55_d9.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen10012015/g1.4_M1.55_d9.png" width="200" /></a>
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen10012015/g1.4_M1.55_d10.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen10012015/g1.4_M1.55_d10.png" width="200" /></a>
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen10012015/g1.4_M1.55_d11.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen10012015/g1.4_M1.55_d11.png" width="200" /></a>
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen10012015/g1.4_M1.55_d12.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen10012015/g1.4_M1.55_d12.png" width="200" /></a>
</p>
<p>
Now increasing d to find regular reflection
</p>
3D Pulsed Jet on DAVinCIehansenTue, 29 Sep 2015 17:35:24 GMT
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen09292015
https://bluehound.circ.rochester.edu/astrobear/blog/ehansen09292015<p>
I tested the new pulsed jet module on Rice's machine DAVinCI, and it seems to work well. This pulsed jet is 3D, MHD, with non-equilibrium cooling.
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen09292015/3Djet_mhd1_rho.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen09292015/3Djet_mhd1_rho.png" width="300" /></a>
</p>
<p>
<a class="attachment" href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen09292015/3Djet_mhd1_rho.gif" title="Attachment '3Djet_mhd1_rho.gif' in Blog: 3D Pulsed Jet on DAVinCI">movie</a><a class="trac-rawlink" href="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen09292015/3Djet_mhd1_rho.gif" title="Download"></a>
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen09292015/3Djet_mhd1_emiss.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen09292015/3Djet_mhd1_emiss.png" width="300" /></a>
</p>
<p>
<a class="attachment" href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen09292015/3Djet_mhd1_emiss.gif" title="Attachment '3Djet_mhd1_emiss.gif' in Blog: 3D Pulsed Jet on DAVinCI">movie</a><a class="trac-rawlink" href="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen09292015/3Djet_mhd1_emiss.gif" title="Download"></a>
</p>
<p>
The code ran pretty well, producing chombos at a steady pace with no restarts. Here are some numbers to show how well this run did on DAVinCI:
</p>
<table class="wiki">
<tr><th> Resolution </th><th> 32 cells/Rjet
</th></tr><tr><th> Cores </th><th> 576
</th></tr><tr><th> Run Time </th><th> 2.5 hrs
</th></tr><tr><th> Cost </th><th> $0.49
</th></tr><tr><th> % Run Completed </th><th> 30%
</th></tr></table>
<p>
The run does slow down as it moves along, so it's hard to say how long the full run would take at this resolution. The code estimates 11.2 more hrs after frame 30, but the actual time is probably closer to 24 hrs. If I assume that the time between chombos grows linearly, then I can estimate the total runtime to be about 24 hours.
</p>
<p>
Thus, the total run at 32 cells/Rjet would take 24 hours on 576 cores, costing 4.70. This is the maximum number of cores that I can use on DAVinCI, and I can only submit for a maximum of 8 hours at a time. So even at this low resolution a run is going to take more than a day if you include wait time and restarting. If we double the resolution to 64 cells/Rjet, this run could take 2 weeks or more instead of 1 day, and the cost would be more than 50.
</p>
<p>
<br />
</p>
<h3 class="section" id="UPDATE">UPDATE</h3>
<p>
Two new models: hydro (no MHD), and an MHD with beta = 1 (same as above) but with precession. Precession amplitude is 3 degrees and the precession frequency is 2.5 times the pulsation frequency.
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen09292015/3Djet_hydro_rho.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen09292015/3Djet_hydro_rho.png" width="200" /></a>
</p>
<p>
<a class="attachment" href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen09292015/3Djet_hydro_rho.gif" title="Attachment '3Djet_hydro_rho.gif' in Blog: 3D Pulsed Jet on DAVinCI">movie</a><a class="trac-rawlink" href="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen09292015/3Djet_hydro_rho.gif" title="Download"></a>
</p>
<p>
<a href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen09292015/3Djet_mhd1_prec_rho.png" style="padding:0; border:none"><img crossorigin="anonymous" src="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen09292015/3Djet_mhd1_prec_rho.png" width="200" /></a>
</p>
<p>
<a class="attachment" href="https://bluehound.circ.rochester.edu/astrobear/attachment/blog/ehansen09292015/3Djet_mhd1_prec_rho.gif" title="Attachment '3Djet_mhd1_prec_rho.gif' in Blog: 3D Pulsed Jet on DAVinCI">movie</a><a class="trac-rawlink" href="https://bluehound.circ.rochester.edu/astrobear/raw-attachment/blog/ehansen09292015/3Djet_mhd1_prec_rho.gif" title="Download"></a>
</p>