Volume 439, Number 2, August IV 2005
|Page(s)||565 - 569|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||29 July 2005|
Limits on the primordial stellar multiplicity
School of Physics & Astronomy, Cardiff University, 5 The Parade, Cardiff CF24 3YB, UK e-mail: Simon.Goodwin@astro.cf.ac.uk
2 Sternwarte, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
3 Rhine Stellar Dynamical Network
Accepted: 10 May 2005
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.
Key words: stars: formation / binaries: general / stars: low-mass, brown dwarfs
© ESO, 2005
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.