Volume 411, Number 2, November IV 2003
|Page(s)||91 - 97|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||17 November 2003|
How do binary separations depend on cloud initial conditions?
European Southern Observatory, Casilla 19001, Santiago 19, Chile
2 Department of Astronomy, SW319, Indiana University, Bloomington, Indiana 47405, USA
3 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
Corresponding author: M. Sterzik, firstname.lastname@example.org
Accepted: 28 August 2003
We explore the consequences of a star formation scenario in which the isothermal collapse of a rotating, star-forming core is followed by prompt fragmentation into a cluster containing a small number () of protostars and/or substellar objects. The subsequent evolution of the cluster is assumed to be dominated by dynamical interactions among cluster members, and this establishes the final properties of the binary and multiple systems. The characteristic scale of the fragmenting core is determined by the cloud initial conditions (such as temperature, angular momentum and mass), and we are able to relate the separation distributions of the final binary population to the properties of the star-forming core. Because the fragmentation scale immediately after the isothermal collapse is typically a factor of 3-10 too large, we conjecture that fragmentation into small clusters followed by dynamical evolution is required to account for the observed binary separation distributions. Differences in the environmental properties of the cores are expected to imprint differences on the characteristic dimensions of the binary systems they form. Recent observations of hierarchical systems, differences in binary characteristics among star forming regions and systematic variations in binary properties with primary mass can be interpreted in the context of this scenario.
Key words: stars: binaries: general / stars: binaries: close / stars: binaries: visual / stars: formation / stars: low-mass, brown dwarfs
© ESO, 2003
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