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The Origin of the Stellar Mass Distribution and Multiplicity

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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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Notes

  1. See Sect. 5.2.1.

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Acknowledgement

We thank the International Space Science Institute (ISSI) for generously providing such stimulating environment for collaboration. Y.N. Lee acknowledges funding from the Ministry of Science and Technology, Taiwan (grant number MOST 108-2636-M-003-001), the grant for Yushan Young Scholar from the Ministry of Education, Taiwan, and the UnivEarthS Labex program at Sorbonne Paris Cité (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02). S.S.R.O. acknowledges funding from NSF Career grant AST-1650486. J.M.D.K. gratefully acknowledges funding from the German Research Foundation (DFG) in the form of an Emmy Noether Research Group (grant number KR4801/1-1) and a DFG Sachbeihilfe Grant (grant number KR4801/2-1), from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme via the ERC Starting Grant MUSTANG (grant agreement number 714907), and from Sonderforschungsbereich SFB 881 “The Milky Way System” (subproject B2) of the DFG. JBP acknowledges UNAM-DGAPA-PAPIIT support through grant number IN-111-219.

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Authors and Affiliations

  1. Department of Earth Sciences, National Taiwan Normal University, 88, Sect. 4, Ting-Chou Road, Taipei City, 11677, Taiwan

    Yueh-Ning Lee

  2. The University of Texas, Austin, TX, 78712, USA

    Stella S. R. Offner

  3. Laboratoire AIM, Paris-Saclay, CEA/IRFU/DAp-CNRS-Université Paris Diderot, 91191, Gif-sur-Yvette Cedex, France

    Patrick Hennebelle & Philippe André

  4. Universidad Autonoma de Chile, Nucleo de Astroquimica y Astrofisica, Avda Pedro de Valdivia 425, Providencia, Santiago de Chile, Chile

    Hans Zinnecker

  5. Instituto de Radioastronomía y Astrofísica, UNAM, Campus Morelia, Antigua Carretera a Patzcuaro 8701, 58090, Morelia, Michoacan, Mexico

    Javier Ballesteros-Paredes

  6. Department of Physics, Nagoya University, Chikusa-ku, Nagoya, 464-8602, Japan

    Shu-ichiro Inutsuka

  7. Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstraße 12-14, 69120, Heidelberg, Germany

    J. M. Diederik Kruijssen

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  1. Yueh-Ning Lee
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Star Formation

Edited by Andrei Bykov, Corinne Charbonnel, Patrick Hennebelle, Alexandre Marcowith, Georges Meynet, Maurizio Falanga and Rudolf von Steiger

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Lee, YN., Offner, S.S.R., Hennebelle, P. et al. The Origin of the Stellar Mass Distribution and Multiplicity. Space Sci Rev 216, 70 (2020). https://doi.org/10.1007/s11214-020-00699-2

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