A Dynamical Origin for Brown Dwarfs
Bo Reipurth, Cathie Clarke, & Eduardo Delgado-Donate
Institute:
Institute for Astronomy, University of Hawaii
Institute:
Institute of Astronomy, University of Cambridge
Contact Email: reipurth@ifa.hawaii.edu
Abstract:
Brown dwarfs may have such low masses because they are prematurely
ejected from small unstable multiple systems, while the members are
still actively building up their masses. We demonstrate that this
scenario is consistent with all currently existing observations of
brown dwarfs, and propose further observational tests. We review the
status of the latest realistic numerical simulations of disintegrating
small N clusters, which show that many of the ejected members end up
with masses that are substellar, drifting away from their birth region
with velocities rarely exceeding 2 km/s.
This paper was withdrawn from the Proceedings.
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Manuscript submitted: 2001-Oct-18
"The Future of Cool-Star Astrophysics", 2003, Eds. A. Brown,
G. M. Harper, & T. R. Ayres.
Proceedings of 12th Cambridge Workshop on Cool Stars, Stellar Systems,
& The Sun,
© 2003 University of Colorado.