Molecular Cloud Fragmentation and Core Collapse

TL;DR

This paper reviews the process of molecular cloud fragmentation leading to star formation, emphasizing the role of magnetic fields and hydrodynamic modeling in different stages of core collapse and disk evolution.

Contribution

It provides a comprehensive overview of molecular cloud fragmentation, highlighting the significance of magnetic fields in early and late stages of star formation.

Findings

Magnetic fields influence cloud fragmentation and core collapse.

Hydrodynamic models help understand disk evolution.

Magnetic control may affect disk formation processes.

Abstract

I review some steps in the conversion of molecular cloud gas into stars and planets, with an emphasis in this presentation on the early stage molecular cloud fragmentation that leads to elongated filaments/ribbons. Magnetic fields can play a crucial role in all stages and need to be invoked particularly for early stage fragmentation as well as in late core collapse where it may control disk formation. I also review some elements of hydrodynamic modeling of disk evolution.