A&A 429, 895-901 (2005)
Kinematics of stars and brown dwarfs at birthE. Moraux and C. Clarke
Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA, UK
(Received 9 June 2004 / Accepted 15 September 2004 )
We use numerical
N-body simulations in order to test whether the
kinematics of stars and brown dwarfs at birth depend on mass. In
particular we examine how initial variations in velocity dispersion
can affect the spatial distribution of stellar and substellar objects
in clusters. We use "toy"
N-body models of a Pleiades-like cluster in
which brown dwarfs have their own velocity dispersion
k times larger than the stellar
We find that in order to match the broad agreement between the brown
dwarf fraction in the field and in the Pleiades, the velocity
dispersion of brown dwarfs at birth has to be less than twice the
stellar velocity dispersion, i.e. cannot exceed a few km s
Pleiades cluster. In order to discern more subtle differences between
the kinematics of brown dwarfs and stars at birth, our simulations show that
we need to look at clusters that are much less dynamically evolved
than the Pleiades. One might especially seek evidence of high velocity
brown dwarfs at birth by examining spatial distribution of stars and
brown darfs in clusters that are about a crossing timescale old.
stellar dynamics --
stars: low-mass, brown dwarfs --
clusters and associations: individual: Pleiades --
stars: kinematics --
© ESO 2005
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