Protostellar angular momentum evolution during gravoturbulent fragmentation

摘要: Using hydrodynamic simulations we investigate the rotational properties and angular momentum evolution of prestellar protostellar cores formed from gravoturbulent fragmentation interstellar gas clouds. We find specific angu- lar j molecular cloud in phase to be on averagej� = 7 × 10 20 cm 2 s −1 our models. This is comparable observed values. A fraction those gravitationally unstable goes into collapse build up protostars systems, which then havej� 8 19 . one order magnitude lower than their parental agreement with observations main-sequence binaries. The loss during mostly due gravitational torques exerted by ambient turbulent flow as well mutual encoun- ters a dense cluster environment. Magnetic are not included models, these would lead even larger transport. ratio energy β that go turns out similar roughly conserved main phase. leads correlation ∝ M 2/3 , between core mass M. Although temporal individual or systems complex highly time-variable, this holds statistical sense for wide range environmental parameters. In addition, high Mach numbers result formation more numerous with, average, mass. Therefore, models momentum. find, however, no dependence spatial scale turbulence. Our predict close vectors neighboring initial accretion Possible observational signatures aligned disks parallel outflows. latter indeed some low-mass isolated Bok globules.