Changes between Version 10 and Version 11 of TriggeredStarFormation


Ignore:
Timestamp:
01/07/14 18:41:52 (11 years ago)
Author:
Shule Li
Comment:

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  • TriggeredStarFormation

    v10 v11  
    1919Simulation lasts till about $4t_{cc}$, which is about 1 million years. The wind should be turned off before that, so we are really looking at an extreme case where the wind lasts for unusually long time. [[BR]]
    2020The simulation box has a resolution of 320 x 192 x 192, with 3 AMR levels of particle refinement. [[BR]]
    21 The following figure shows the at 0.6 million years. (a) non-rotation Mach 1.5(case N), (b) non-rotation Mach 3.16(case N'), (c) parallel rotation Mach 1.5(case R1), (d) perpendicular rotation Mach 1.5(case R2).[[BR]][[BR]]
     21The following figure shows the column density for different cases at 0.6 million years. (a) non-rotation Mach 1.5(case N), (b) non-rotation Mach 3.16(case N'), (c) parallel rotation Mach 1.5(case R1), (d) perpendicular rotation Mach 1.5(case R2).[[BR]][[BR]]
    2222[[BR]][[BR]]
    2323[[Image(fig2.png,60%)]]
    … …  
    3939http://www.pas.rochester.edu/~shuleli/tsf_paper/perrot.gif
    4040[[BR]]
    41 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:
    42 [[BR]]
     41Generally, 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 density comparison (slice through the center) is shown in the following figure: [[BR]][[BR]]
     42
     43[[Image(http://www.pas.rochester.edu/~shuleli/0321/tsf_comparison.png,40%)]]
     44[[BR]][[BR]]
     45
     46The 3D rendering of cloud material tracer for case R1, is as follows:
     47[[BR]][[BR]]
    4348[[Image(http://www.pas.rochester.edu/~shuleli/tsf_paper/paper_figs/fig1.png, 40%)]]
    4449[[BR]][[BR]]
    … …  
    9196
    9297'''MHD Triggering'''[[BR]]
    93 When added magnetic field to the cloud, the triggering behavior can be very different. Here, we suppose the initial rotation to be zero first, and look at the case where there is a global uniform magnetic field along .
     98When added magnetic field to the cloud, the triggering behavior can be very different. Here, we suppose the initial rotation to be zero first, and look at the case where there is a global uniform magnetic field along the vertical axis. We assume Mach = 3, and the magnetic field has beta of 4. The density slice looks like:[[BR]][[BR]]
     991 cloud crushing time: [[BR]]
     100[[Image(http://www.pas.rochester.edu/~shuleli/0321/tsfmach36v_0017.png,40%)]]
     101[[BR]][[BR]]
     1022.5 cloud crushing time: [[BR]]
     103[[Image(http://www.pas.rochester.edu/~shuleli/0321/tsfmach36v_0041.png,40%)]]
     104[[BR]][[BR]]
     105Density slice movie:[[BR]]
     106http://www.pas.rochester.edu/~shuleli/0321/tsfmach36v.gif
     107[[BR]][[BR]]
     108Column density movie: [[BR]]
     109http://www.pas.rochester.edu/~shuleli/0323/mach3bcd.gif
     110[[BR]][[BR]]
     111
     112Next, we study if the field is contained within the cloud. We divide the simulations into categories where the contained field is either poloidal or toroidal, and look at the triggering behavior when the poloidal or toroidal axis is parallel or perpendicular to the incoming shock. As shown in our earlier paper about shock interaction with a magnetized clump, it is possible to form multiple compression cores in such a scenario. One natural question is, can we have formation of more than one stars within a single magnetized cloud? The following cut is taken from a simulation where the poloidal field has a maximum strength of beta = 1, incoming shock Mach = 1.5. We plot the column density as well as the 1/beta parameter (in the smaller frame).[[BR]][[BR]]
     113[[Image(http://www.pas.rochester.edu/~shuleli/mhdtsf/mhd_poloidal.png,70%)]]
     114[[BR]][[BR]]
     115The following figure is the toroidal field case:[[BR]][[BR]]
     116[[Image(http://www.pas.rochester.edu/~shuleli/mhdtsf/mhd_toroidal.png,70%)]]
     117[[BR]][[BR]]
     118Movies:[[BR]]
     119Poloidal contained field:[[BR]]
     120http://www.pas.rochester.edu/~shuleli/mhdtsf/tsfpol.gif
     121[[BR]]
     122Toroidal contained field:[[BR]]
     123http://www.pas.rochester.edu/~shuleli/mhdtsf/tsftor.gif
     124[[BR]]
    94125
    95126
    96127
    97 Next, we study if the field is contained within the cloud. We divide the simulations into categories where the contained field is either poloidal or toroidal, and look at the triggering behavior when the poloidal or toroidal axis is parallel or perpendicular to the incoming shock. As shown in our earlier paper about shock interaction with a magnetized clump, it is possible to form multiple compression cores in such a scenario. One natural question is, can we have formation of more than one stars within a single magnetized cloud?[[BR]]
    98128
    99129
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     131