Changes between Version 24 and Version 25 of GravoTurbulence
- Timestamp:
- 11/13/11 00:28:09 (13 years ago)
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GravoTurbulence
v24 v25 1 [[PageOutline]] 1 2 = Gravo-Turbulence = 2 3 … … 18 19 19 20 Most of these had densities of at least 800 (twice the mean) with several having densities of 1600 and a few with densities of 3200. The ones with a density of 800 would be stable to collapse and those with a density of 1600 have Jeans lengths of .26 pc and could potentially collapse - although the timescales would be similar to the timescales for the global collapse. This is in fact what we see... Two particles form before the entire thing collapses and then forms a binary system with periodic ejections of material. Not sure if this is a protection issue, or material being slingshotted from the secondary. Eventually the particles become unbound and begin to seemingly accelerate upwards. This may be related to the way periodic BC's handle self gravity (which won't be a problem in 3D), or may be related to the particle kick #157. 20 21 Below is the initial density perturbation and here is the [attachment:collapse.gif movie] 22 23 [[Image(collapse.png, width=400)]] 24 25 26 27 So i modified the mean density to be 10, set [[latex($\alpha=-2$)]] so [[latex($\beta-1$)]] and strengthened the perturbation. Below is the initial density perturbation and here is the [attachment:hires.gif movie] 28 29 [[Image(hires.png, width=400)]] 21 === I === 22 || I || 23 || [[Image(collapse.png, width=400)]] || 24 || [attachment:collapse.gif movie] || 25 26 27 So i modified the mean density to be 10, set [[latex($\alpha=-2$)]] so [[latex($\beta-1$)]] and strengthened the perturbation. 28 29 === II === 30 || II || 31 || [[Image(hires.png, width=400)]] || 32 || [attachment:hires.gif movie] || 33 34 30 35 31 36 … … 45 50 If instead the gas is at the same temperature everywhere, then initial differences in density will cause expansion 46 51 47 [[Image(MultiPoleCollapse.png, width=400)]] 48 49 [attachment:MultiPoleCollapse.gif movie] 52 === III === 53 || III || 54 || [[Image(MultiPoleCollapse.png, width=400)]] || 55 || [attachment:MultiPoleCollapse.gif movie] || 50 56 51 57 … … 89 95 || t,,ff,, || 11.2 Myr || 90 96 || L,,J,, || 30 pc || 91 92 93 [[Image(MPCollBig.png, width=400)]] 94 95 [attachment:MPCollBig.gif movie] 97 === IV === 98 || IV || 99 || [[Image(MPCollBig.png, width=400)]] || 100 || [attachment:MPCollBig.gif movie] || 96 101 97 102 … … 111 116 112 117 Here is another movie of density that zooms in as the cloud collapses. A few bugs were fixed and phi-gradient refinement was used and there is no longer an explosion... 113 114 [[Image(ZoomingRhoTestwSinksLong.png, width=400)]] 115 116 [attachment:ZoomingRhoTestwSinksLong.gif movie] 118 === IVb === 119 || IVb || 120 || [[Image(ZoomingRhoTestwSinksLong.png, width=400)]] || 121 || [attachment:ZoomingRhoTestwSinksLong.gif movie] || 117 122 118 123 … … 145 150 146 151 If the kinetic energy is put into solenoidal motions with a spectral index [[latex($\alpha = -1$)]] so that [[latex($\hat{v}(k)\propto k^{\alpha}$)]], then energy dissipates fairly quickly and the whole thing collapses 147 148 149 [[Image(MPCollVir.png, width=400)]] 150 151 [attachment:MPCollVir.gif movie] 152 === V === 153 || V || 154 || [[Image(MPCollVir.png, width=400)]] || 155 || [attachment:MPCollVir.gif movie] || 152 156 153 157 154 158 And here is another movie with phi-gradient refinement and with a steeper initial velocity profile [[latex($\hat{v}(k)\propto k^{-3/2}$)]] so that [[latex($E_{1D}(k) \propto k^{-2}$)]] 155 156 [[Image(LargeScaleDriving.png, width=400)]] 157 158 [attachment:LargeScaleDriving.gif movie] 159 === VI === 160 || VI || 161 || [[Image(LargeScaleDriving.png, width=400)]] || 162 || [attachment:LargeScaleDriving.gif movie] || 159 163 160 164 And here is a movie showing cloud temperature early on. You can see the dense filaments cool to 10K. 161 162 [[Image(2DCloudTemp.png, width=400)]] 165 || VI || 166 || [[Image(2DCloudTemp.png, width=400)]] || 163 167 164 168
