From Molecular Clouds to the IMF: Spatial and Temporal Effects

TL;DR

This paper reviews star formation in molecular clouds, emphasizing magnetic fields' roles, filamentary structures, and the origin of the IMF, proposing a mathematical model linking accretion to stellar mass distribution.

Contribution

It introduces a modified lognormal power-law (MLP) model to connect accretion processes with the initial mass function (IMF).

Findings

Magnetic fields influence filamentary structures and density PDFs.

The MLP model offers a new framework for understanding the IMF.

Explanations beyond Jeans length are needed for the IMF origin.

Abstract

We review star formation in molecular clouds and describe why magnetic fields may be important and how they can influence filamentary structure and the column density probability distribution function (PDF). We also comment on the origin of the stellar and substellar initial mass function (IMF), which may require explanations beyond a simple Jeans length argument in turbulent molecular clouds. A mathematical model of the modified lognormal power-law (MLP) distribution function provides a framework within which to connect accretion processes with the IMF.