Protostellar disk accretion in turbulent filaments
Astronomy & Astrophysics(2024)
摘要
Recent observations of protostellar cores suggest that most of the material
in the protostellar phase is accreted along streamers. Streamers in this
context are defined as velocity coherent funnels of denser material potentially
connecting the large scale environment to the small scales of the forming
accretion disk. Using simulations which simultaneously resolve the driving of
turbulence on the filament scale as well as the collapse of the core down to
protostellar disk scales, we aim to understand the effect of the turbulent
velocity field on the formation of overdensities in the accretion flow. We
perform a three-dimensional numerical study on a core collapse within a
turbulent filament using the RAMSES code and analyse the properties of
overdensities in the accretion flow. We find that overdensities are formed
naturally by the initial turbulent velocity field inherited from the filament
and subsequent gravitational collimation. This leads to streams which are not
really filamentary but show a sheet-like morphology. Moreover, they have the
same radial infall velocities as the low density material. As a main
consequence of the turbulent initial condition, the mass accretion onto the
disk does not follow the predictions for solid body rotation. Instead, most of
the mass is funneled by the overdensities to intermediate disk radii.
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