Changes between Version 37 and Version 38 of AstroBearProjects/MagnetizedClumps
- Timestamp:
- 01/07/14 21:16:49 (11 years ago)
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AstroBearProjects/MagnetizedClumps
v37 v38 38 38 39 39 The image below shows the clump evolution when the uniform magnetic field is perpendicular to the shock direction.[[BR]][[BR]] 40 [[Image(perpfield1.png, 40 [[Image(perpfield1.png,30%)]][[BR]][[BR]] 41 41 1. The magnetic field is stretched and wrapped around the clump, which effectively confines the clump and prevents its fragmentation, even for moderately strong field β = 4. The clump [[BR]] 42 42 embedded in the stretched field is compressed, but then, because of the strong confining effect of the field develops a streamlined profile and is not strongly eroded. [[BR]] … … 47 47 aligned field case. [[BR]][[BR]] 48 48 49 50 51 49 In AstroBEAR, the clump simulation is done using the clump object, the wind object and the cooling object. We also implement various multiphysics processes to make the situation [[BR]] 52 50 more interesting. Below are snapshots of the clump density and magnetic pressure in a 3-D AMR simulation. Notice the field concentration at [[latex($\tau_{cc}$)]] is very different for [[BR]] 53 51 the aligned and perpendicular field cases. [[BR]][[BR]] 54 [[Image(comparisonamr.png, 52 [[Image(comparisonamr.png,40%)]][[BR]][[BR]] 55 53 [http://http://www.pas.rochester.edu/~shuleli/clumpview/trial.gif Here is a movie of the mentioned simulation.][[BR]][[BR]] 56 54 57 55 The following images show the high resolution shocked clump problem with uniform magnetic field in AMR. [[BR]][[BR]] 58 [[Image(alignedstrong.png, 30%)]][[Image(perpweak.png, 30%)]][[Image(perpstrong.png,30%)]][[BR]][[BR]]56 [[Image(alignedstrong.png,30%)]][[Image(perpweak.png,30%)]][[Image(perpstrong.png,30%)]][[BR]][[BR]] 59 57 58 == Shock Clumps Interaction with Contained Magnetic Field == 59 Here we study the shock interaction with the clump when the clump has tangled magnetic field contained. We focus on the following 4 cases:[[BR]] 60 [[Image(fig02_rev_color.png)]][[BR]][[BR]] 61 The contained magnetic field has a volume-average beta of 0.25. The volume rendered results for the four cases (the four columns for TA, TP, PA, PP cases, respectively). Each row corresponds to 1, 2 and 3.5 cloud crushing time.[[BR]] 62 [[Image(fig03_rev_color.png)]][[Image(fig04_rev_color.png)]][[Image(fig05_rev_color.png)]][[Image(fig06_rev_color.png)]][[BR]][[BR]] 63 Movies:[[BR]] 64 TA case:[[BR]] 65 http://www.pas.rochester.edu/~shuleli/HedlaMovie/torxvr.gif 66 [[BR]] 67 TP case:[[BR]] 68 http://www.pas.rochester.edu/~shuleli/HedlaMovie/torzvr.gif 69 [[BR]] 70 PA case:[[BR]] 71 http://www.pas.rochester.edu/~shuleli/HedlaMovie/polzvr.gif 72 [[BR]] 73 PP case:[[BR]] 74 http://www.pas.rochester.edu/~shuleli/HedlaMovie/polxvr.gif 75 [[BR]][[BR]] 76 The magnetic field intensity map is plotted as follows:[[BR]][[BR]] 77 [[Image(fig11_rev_bw.png,50%)]][[BR]][[BR]] 78 79 The contained magnetic field geometry can influence the kinetic and magnetic energy evolution. As shown in the following plot:[[BR]][[BR]] 80 [[Image(fig12_rev_bw.png,50%)]][[BR]] 81 [[Image(fig13_rev_bw.png,50%)]][[BR]][[BR]] 82 The wind-clump mixing ratio can be affected also by the contained field geometry, as the toroidal contained field can enhance the clump edges to resist the instability erosion. [[BR]] 83 [[Image(fig14.png,50%)]][[BR]] 84 [[Image(fig15.png,50%)]][[BR]][[BR]] 85 86 Mixing Ratio Evolution Movies:[[BR]] 87 Strong contained field (average beta of 0.25)[[BR]] 88 http://www.pas.rochester.edu/~shuleli/movie0703/mrst.gif 89 [[BR]][[BR]] 90 Weak contained field (average beta of 1)[[BR]] 91 http://www.pas.rochester.edu/~shuleli/movie0703/mrwk.gif 92 [[BR]][[BR]] 93 94 The mathematical model that can qualitatively explain the line plots is available in the paper:[[BR]] 95 96 [[BR]][[BR]] 60 97 == Presentations == 61 98 … … 67 104 http://arxiv.org/abs/0707.2616 68 105 http://arxiv.org/abs/1003.5546 69 70 71
