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Title:
Limits on the primordial stellar multiplicity
Authors:
Goodwin, S. P.; Kroupa, P.
Affiliation:
AA(School of Physics and Astronomy, Cardiff University, 5 The Parade, Cardiff CF24 3YB, UK ), AB(Sternwarte, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany; Rhine Stellar Dynamical Network)
Publication:
Astronomy and Astrophysics, Volume 439, Issue 2, August IV 2005, pp.565-569 (A&A Homepage)
Publication Date:
08/2005
Origin:
EDP Sciences
Astronomy Keywords:
stars: formation, binaries: general, stars:, low-mass, brown dwarfs
DOI:
10.1051/0004-6361:20052654
Bibliographic Code:
2005A&A...439..565G

Abstract

Most stars - especially young stars - are observed to be in multiple systems. Dynamical evolution is unable to pair stars efficiently, which leads to the conclusion that star-forming cores must usually fragment into ≥ 2 stars. However, the dynamical decay of systems with ≥ 3 or 4 stars would result in a large single-star population that is not seen in the young stellar population. Additionally, ejections would produce a significant population of close binaries that are not observed. This leads to a strong constraint on star formation theories that cores must typically produce only 2 or 3 stars. This conclusion is in sharp disagreement with the results of currently available numerical simulations that follow the fragmentation of molecular cores and typically predict the formation of 5-10 seeds per core. In addition, open cluster remnants may account for the majority of observed highly hierarchical higher-order multiple systems in the field.
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