| | 322 | * What is their IMF or CMF? |
| | 323 | |
| | 324 | = [http://arxiv.org/pdf/1107.3616v1.pdf Clustered Star Formation in Magnetic Clouds: Properties of Dense Cores Formed in Outflow-Driven Turbulence] (Nakamura & Li) = |
| | 325 | |
| | 326 | |
| | 327 | * 1.5 pc box with a 939 M,,solar,, core |
| | 328 | * [[latex($\alpha_{vir}=.5$)]] |
| | 329 | * Initial turbulence is imposed with v,,k,, ~ k^-4^ and allowed to decay |
| | 330 | * Stars that form inject momenta proportional to accretion rate back into surrounding gas |
| | 331 | * 3 simulations at 256^3^ |
| | 332 | * [[latex($\beta = \infty$)]] (N) |
| | 333 | * [[latex($\beta = 2$)]] (W) |
| | 334 | * [[latex($\beta = .2$)]] (S) (initial virial equilibrium with turbulence) |
