The Origin of the Stellar Mass Distribution and Multiplicity
Yueh-Ning Lee, Stella S.R. Offner, Patrick Hennebelle, Philippe, Andr\'e, Hans Zinnecker, Javier Ballesteros-Paredes, Shu-ichiro Inutsuka, and, J.M. Diederik Kruijssen
TL;DR
This paper reviews the historical and recent understanding of the Initial Mass Function and Core Mass Function, emphasizing star formation in clusters, gas fragmentation, and binary system formation.
Contribution
It provides a comprehensive overview of observational and theoretical advances in star formation, focusing on mass distribution and multiplicity in clustered environments.
Findings
Turbulent gas fragmentation influences star mass distribution.
Binary and multiple star systems form through specific fragmentation processes.
Recent models better explain the observed stellar mass functions.
Abstract
In this chapter, we review some historical understanding and recent advances on the Initial Mass Function (IMF) and the Core Mass Function (CMF), both in terms of observations and theories. We focus mostly on star formation in clustered environment since this is suggested by observations to be the dominant mode of star formation. The statistical properties and the fragmentation behaviour of turbulent gas is discussed, and we also discuss the formation of binaries and small multiple systems.
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