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Koronis family members (circles) projected on the plane of
proper semimajor axis and proper eccentricity; Karin cluster is indicated
in the lower right corner. For an isotropic velocity field, and different
values of orbital parameters, ejecta from a hypothetical secondary collision
near (2953) Vysheslavia (full circle) would fall in the region indicated
by dots. None of the observed Koronis asteroids falls in this zone,
notably in its stable part above the 5/2 mean motion resonance with Jupiter.
%
Orbital stability is indicated by color shading obtained by means of
a parameter $\sigma = 1 - n^{(2)}/n^{(1)}$, where $n^{(1)}$ and $n^{(2)}$
are proper mean motions of test particles calculated in the two consequtive
time intervals, each spanning 1.2~Myr.
%
The family members were identified using the hierarchical clustering
method and the velocity cutoff of $60$~m/s, e.g. Zappal\`a
{\it et~al.} (1995), Bottke {\it et~al.} (2001). At first, we used
the catalogue of proper elements (Kne\v zevi\'c and Milani 2003) 
computed analytically for the identification process. Then we selected
(and plotted) those asteroids, which have synthetic proper elements,
since proper elements of our test particles are computed with
a similar algorithm.

\begin{thebibliography}{}
\bibitem[Kne\v zevi\'c and Milani 2003]{kne03} Kne\v zevi\'c, Z., A. Milani
 2003. Proper elements.
 In {\it Asteroids~III}
 (W.F. Bottke, A. Cellino. P. Paolicchi and R. Binzel, Eds.) 
 pp.~395--408. University of Arizona Press, Tucson.
\end{thebibliography}

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