The Origin of the Stellar Mass Distribution and Multiplicity
- PDF / 3,322,110 Bytes
- 56 Pages / 439.37 x 666.142 pts Page_size
- 32 Downloads / 171 Views
The Origin of the Stellar Mass Distribution and Multiplicity Yueh-Ning Lee1 · Stella S.R. Offner2 · Patrick Hennebelle3 · Philippe André3 · Hans Zinnecker4 · Javier Ballesteros-Paredes5 · Shu-ichiro Inutsuka6 · J.M. Diederik Kruijssen7
Received: 3 February 2020 / Accepted: 29 May 2020 © Springer Nature B.V. 2020
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. Star Formation Edited by Andrei Bykov, Corinne Charbonnel, Patrick Hennebelle, Alexandre Marcowith, Georges Meynet, Maurizio Falanga and Rudolf von Steiger
B Y.-N. Lee
[email protected] S.S.R. Offner [email protected] P. Hennebelle [email protected] P. André [email protected] H. Zinnecker [email protected] J. Ballesteros-Paredes [email protected] S.-i. Inutsuka [email protected] J.M.D. Kruijssen [email protected]
1
Department of Earth Sciences, National Taiwan Normal University, 88, Sect. 4, Ting-Chou Road, Taipei City 11677, Taiwan
2
The University of Texas, Austin, TX 78712, USA
3
Laboratoire AIM, Paris-Saclay, CEA/IRFU/DAp-CNRS-Université Paris Diderot, 91191 Gif-sur-Yvette Cedex, France
70
Page 2 of 56
Y.-N. Lee et al.
Keywords Initial mass function · Core mass function · Stellar cluster · Multiplicity
1 Introduction Stars form in regions where a sufficient amount of mass is concentrated, reaching densities that allow gravitational collapse to overcome all possible supporting agents such as thermal and radiative pressure, turbulence, and magnetic fields. When such conditions are reached, the amount of mass usually allows a group of stars to form together, which is indeed supported by observations (Lada and Lada 2003; Kruijssen 2012; Longmore et al. 2014). Moreover, gravitational collapse is hierarchical and often leads to fragmentation across a range of size scales (Efremov and Elmegreen 1998; Hopkins 2013a; Vázquez-Semadeni et al. 2017; Pokhrel et al. 2018; Vázquez-Semadeni et al. 2019). Therefore, from the largest-scale entities that contain thousands to millions of star to small multiple or binary systems, there is always a certain degree of grouping, or clustering, when star formation takes place. In other words, stars that form in isolation represent a very small proportion. Given a group of stars, statistical properties can be inferred, in particular that of the stellar mass, which is the primary parameter of a star. A star’s mass at birth, or “initial stellar mass,” determines how it will evolve, the way it interacts with its environment, how long it will live and the mechanism by which it will eventually die. The mass of members of a stella
Data Loading...
