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Stellar and brown dwarf properties from numerical simulations

Published online by Cambridge University Press:  21 October 2010

Matthew R. Bate
Matthew R. Bate*
Affiliation:
School of Physics, University of Exeter Stocker Road, Exeter EX4 4QL, United Kingdom email: mbate@astro.ex.ac.uk
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Abstract

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We review the statistical properties of stars and brown dwarfs obtained from the first hydrodynamical simulation of star cluster formation to produce more than a thousand stars and brown dwarfs while simultaneously resolving the lowest mass brown dwarfs (those with masses set by the opacity limit for fragmentation), binaries with separations down to ~ 1 AU, and discs with radii greater than ~ 10 AU. In particular, we present the eccentricity distribution of the calculation's very-low-mass and brown dwarf binaries which has not been previously published.

Keywords

gravitationhydrodynamicsstellar dynamicsmethods: numericalbinaries: generalstars: formationstars: low-massbrown dwarfsstars: luminosity functionmass function
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 769 - 770
Copyright
Copyright © International Astronomical Union 2010

References

Bate, M. R. 2009a, MNRAS, 392, 590CrossRefGoogle Scholar
Bate, M. R. 2009b, MNRAS, 392, 1363CrossRefGoogle Scholar