The Origins of Protostellar Core Angular Momenta

Abstract

We present the results of a suite of numerical simulations designed to explore the origin of the angular momenta of protostellar cores. Using the hydrodynamic grid code \emph{Athena} with a sink implementation, we follow the formation of protostellar cores and protostars (sinks) from the subvirial collapse of molecular clouds on larger scales to investigate the range and relative distribution of core properties. We find that the core angular momenta are relatively unaffected by large-scale rotation of the parent cloud; instead, we infer that angular momenta are mainly imparted by torques between neighboring mass concentrations and exhibit a log-normal distribution. Our current simulation results are limited to size scales $\sim 0.05$~pc ($\sim 10^4\mathrm{AU}$), but serve as first steps toward the ultimate goal of providing initial conditions for higher-resolution studies of core collapse to form protoplanetary disks.

arXiv comment12 pages, 9 figures, accepted to ApJ

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• Investigating the Complex Velocity Structures within Dense Molecular Cloud Cores with GBT-Argus
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• Mergers of Equal-Mass Binaries with Compact Object Companions from Mass Transfer in Triple Star Systems
• Protostellar disk formation by a non-rotating, non-axisymmetric collapsing cloud: model and comparison with observations
• Evolution of the Angular Momentum of Molecular Cloud Cores Formed from Filament Fragmentation
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• Collapsing Molecular Clouds with Tracer Particles: Part I, What Collapses?
• Infall and Disk Processes - the Message from Meteorites
• Touching the Stars: Using High-Resolution 3D Printing to Visualize Stellar Nurseries