| 2 | |
| 3 | The goal is to study how different initial conditions lead to a state of gravitational collapse and characterize the turbulence and to either back-out how viable formation mechanisms for MC's or determine that IC's are not important to MC evolution. |
| 4 | |
| 5 | Possible different IC's to use: |
| 6 | * Pure density perturbations (with either an Isothermal eq of state - or IICooling to trigger thermal instabilities) |
| 7 | * Initial solenoidal velocity fields (virial equilibrium) |
| 8 | * Compressive flows (2 finite streams)? |
| 9 | * Magnetically critical clouds |
| 10 | |
| 11 | |
| 12 | == Density Perturbations == |
| 13 | Goal is to put a cloud with random perturbations following a given power spectra [[latex($P_\xi(k)=Ak^\beta$)]] for [[latex($k_{\min} <= k <= k_{\max}$)]] where [[latex($\xi=\log(\rho)$)]]. The perturbations will be windowed on a region with a finite radius embedded in a much lower density region. Since [[latex($\int{P_\xi(k)dk} = \int{\hat{\xi}(k)k^2dk}$)]] we must have [[latex($\hat{\xi}(k) \propto k^\alpha$)]] where [[latex($\alpha = \beta-2$)]] |
| 14 | |
| 15 | == Velocity Perturbations == |
| 16 | |
| 17 | |