The Origin of the Stellar Mass Distribution and Multiplicity

Lee, Yueh-Ning; Offner, Stella S. R.; Hennebelle, P.; André, P.; Zinnecker, H.; Ballesteros-Paredes, Javier; Inutsuka, S.; Kruijssen, J. M. Diederik

doi:10.1007/s11214-020-00699-2

Cited by 44 publications

(38 citation statements)

References 361 publications

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“…Continued accretion on to newly formed binaries shrinks their orbits [6,38]. The origins of the stellar mass distribution (the initial mass function, IMF, and the system mass function, SMF) and its relation to multiplicity are reviewed by Lee et al [39]. The SMF can be explained because of the mass distribution of prestellar cores (if a given fraction of the core mass is converted into stars), or as a result of competitive accretion.…”

Section: Physics Of Star Formationmentioning

confidence: 99%

Architecture of Hierarchical Stellar Systems and Their Formation

Tokovinin

2021

Universe

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Accumulation of new data on stellar hierarchical systems and the progress in numerical simulations of their formation open the door to genetic classification of these systems, where properties of a certain group (family) of objects are tentatively related to their formation mechanisms and early evolution. A short review of the structure and statistical trends of known stellar hierarchies is given. Like binaries, they can be formed by the disk and core fragmentation events happening sequentially or simultaneously and followed by the evolution of masses and orbits driven by continuing accretion of gas and dynamical interactions between stars. Several basic formation scenarios are proposed and associated qualitatively with the architecture of real systems, although quantitative predictions for these scenarios are still pending. The general trend of increasing orbit alignment with decreasing system size points to the critical role of the accretion-driven orbit migration, which also explains the typically comparable masses of stars belonging to the same system. The architecture of some hierarchies bears imprints of chaotic dynamical interactions. Characteristic features of each family are illustrated by several real systems.

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Section: Physics Of Star Formationmentioning

confidence: 99%

Architecture of Hierarchical Stellar Systems and Their Formation

Tokovinin

2021

Universe

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“…Turbulence is a common feature of present day giant molecular clouds in which star formation is clearly evident (e.g. Girichidis et al 2020;Lee et al 2020;Krause et al 2020) and while in both cases the gas is moving super-sonically the coolants available to the gas in both cases make direct comparisons difficult. After approximately 2 Myr the stars in HaloA will start to directly collapse in black holes retaining close to 100% of the stellar mass (Heger et al 2003).…”

Section: Discussionmentioning

confidence: 99%

The Formation of Very Massive Stars in Early Galaxies and Implications for Intermediate Mass Black Holes

Regan¹,

Wise²,

Woods³

et al. 2020

TheOJA

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“…The binary formation mechanism must be able to explain the range of observed separations and the observed mass ratio distribution among binary systems. Lee et al (2020) presents a discussion of theoretical models. Suggested mechanisms are turbulent fragmentation of a core, the gravitational fragmentation of an unstable accretion disk, or gravitational capture during dynamical interactions.…”

Section: Binary Formation Mechanismsmentioning

confidence: 99%

“…Bergfors et al (2010) estimated the multiplicity fraction of 34% between 0.08-0.45 M , suggesting a decreasing fraction of binary stars with mass. A recent review by Lee et al (2020) presents our current understanding of binary and multiple systems in the Galactic field, along with a comprehensive review of estimations of BF across a range of mass. Parker & Meyer (2014) suggested that the binary population in the field is indicative of the primordial binary population in star-forming regions, at least for systems with primary masses in the range 0.02--3.0 M .…”

Section: Introductionmentioning

confidence: 99%

High Mass-ratio Binary Population in Open Clusters: Segregation of early type binaries and an increasing binary fraction with mass

Jadhav,

Roy,

Joshi

et al. 2021

Preprint

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Binary stars play a vital role in astrophysical research, as a good fraction of stars are in binaries. Binary fraction (BF) is known to change with stellar mass in the Galactic field, but such studies in clusters require binary identification and membership information. Here, we estimate the total and spectral-type-wise high mass-ratio (HMR) BF (f 0.6 ) in 23 open clusters using unresolved binaries in color-magnitude diagrams using Gaia DR2 data. We introduce the segregation index (SI) parameter to trace mass segregation of HMR (total and mass-wise) binaries and the reference population. This study finds that in open clusters, (1) HMR BF for the mass range 0.4-3.6 M (early M to late B type) has a range of 0.12 to 0.38 with a peak at 0.12-0.20, (2) older clusters have a relatively higher HMR BF, (3) the mass-ratio distribution is unlikely to be a flat distribution and BF(total) ∼ (1.5 to 2.5) ×f 0.6 , (4) a decreasing BF(total) from late B-type to K-type, in agreement with the Galactic field stars, (5) older clusters show radial segregation of HMR binaries, (6) B and A/F type HMR binaries show radial segregation in some young clusters suggesting a primordial origin. This study will constrain the initial conditions and identify the major mechanisms that regulate binary formation in clusters. Primordial segregation of HMR binaries could result from massive clumps spatially segregated in the collapse phase of the molecular cloud.

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The Origin of the Stellar Mass Distribution and Multiplicity

Cited by 44 publications

References 361 publications

Architecture of Hierarchical Stellar Systems and Their Formation

Architecture of Hierarchical Stellar Systems and Their Formation

The Formation of Very Massive Stars in Early Galaxies and Implications for Intermediate Mass Black Holes

High Mass-ratio Binary Population in Open Clusters: Segregation of early type binaries and an increasing binary fraction with mass

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