Changes between Version 1 and Version 2 of TriggeredStarFormation
- Timestamp:
- 01/07/14 18:07:21 (11 years ago)
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TriggeredStarFormation
v1 v2 20 20 The following figure shows the at 0.6 million years. [[BR]][[BR]] 21 21 [[BR]][[BR]] 22 22 [[Image(fig2.png)]] 23 [[BR]][[BR]] 23 24 Movies:[[BR]] 24 25 Case N: [[BR]] … … 38 39 [[BR]] 39 40 Generally, the evolution can be divided into three stages: As we can see the two rotating cases develop disks with the axis aligned with the initial rotation. The 3D rendering of cloud material tracer for case R1, is as follows: 41 [[BR]] 42 [[Image(http://www.pas.rochester.edu/~shuleli/tsf_paper/paper_figs/fig1.png, 40%)]] 40 43 [[BR]][[BR]] 41 44 42 45 We can study important physics quantities by line plots. The first set of line plots are 1. star mass formed by triggering, 2. accretion rate, 3. mixing ratio of the wind material onto the star, 4. bounded mass (basically the mass of the disk for the rotation cases. for the non-rotating cases, the bounded material evaporates very fast after stage I. [[BR]] 43 [[Image( http://www.pas.rochester.edu/~shuleli/tsf_paper/paper_figs/fig1.png, 40%)]]46 [[Image(fig4.png)]] 44 47 [[BR]][[BR]] 45 48 … … 83 86 84 87 85
