# The Origins of Protostellar Core Angular Momenta

## TL;DR

This study uses numerical simulations to investigate the origins of angular momentum in protostellar cores, finding that local torques rather than large-scale cloud rotation primarily impart angular momentum.

## Contribution

The paper introduces simulation results showing that protostellar core angular momentum is mainly due to local torques, not large-scale cloud rotation, advancing understanding of core formation processes.

## Key findings

- Core angular momenta are unaffected by large-scale cloud rotation.
- Angular momenta are mainly imparted by torques between neighboring mass concentrations.
- Core angular momentum distribution follows a log-normal pattern.

## 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 ($\sim 10^4 \rm AU$), but serve as first steps toward the ultimate goal of providing initial conditions for higher-resolution studies of core collapse to form protoplanetary disks.