Changes between Version 28 and Version 29 of AstroBearProjects/MagnetizedClumps
- Timestamp:
- 02/13/12 22:50:16 (13 years ago)
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AstroBearProjects/MagnetizedClumps
v28 v29 20 20 It also serves as an example on clumps getting shocked with 2-D uniform magnetic field.[[BR]] 21 21 The image below shows the clump evolution when the uniform magnetic field is aligned with the shock direction.[[BR]][[BR]] 22 22 [[Image(alignedfield1.png, 40%)]][[BR]][[BR]] 23 23 24 24 In these simulations we notice:[[BR]] … … 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 40 [[Image(perpfield1.png, 40%)]][[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]] … … 52 52 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 53 the aligned and perpendicular field cases. [[BR]][[BR]] 54 54 [[Image(comparisonamr.png, 40%)]][[BR]][[BR]] 55 55 56 56 Here is a movie of the mentioned simulation. [[BR]][[BR]]
