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REFERENCES
J
case clearly show that
some bodies further than ~2
from the relation
are present. We suggest, therefore, that the
minor planets in the outer belt with short T
L
(and T
e
< T
SS
) are the counterparts of these
bodies for the real, 1 M
J
case.
We thank Brian Marsden and Gareth
Williams of the Minor Planet Center for their
usual cheerful and prompt responses to
requests for asteroid ephemerides.
Chaotic Motion in the Outer Asteroid Belt
page 13
