Angular Momentum Evolution from Core to Disk Scales in the Early Phase of Star Formation: Constraints from HH 212, HH 211, and B335

arXiv:2607.28056 · astro-ph.GA · Submitted 2026-07-30 · Read on arXiv

Chin-Fei Lee

astro-ph.GA

Submitted: 2026-07-30

Comments: 16 pages, 2 figures

License: http://arxiv.org/licenses/nonexclusive-distrib/1.0/

Terminology

• Core — 75× in this paper · explained in 2 episodes
• Ambipolar Diffusion — 2× in this paper · explained in 1 episode
• Angular Momentum Transport — 2× in this paper · explained in 3 episodes
• Trace — 2× in this paper · explained in 2 episodes
• Angular Momentum Loss — 1× in this paper · explained in 1 episode
• Consistency — 1× in this paper · explained in 3 episodes
• Unified Framework — 1× in this paper · explained in 5 episodes

Sources

• Modelling the Break in the Specific Angular Momentum within the Envelope-Disk Transition Zone
• The role of magnetic fields in the formation of protostars, disks, and outflows

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