  We studied impact processes by means of smoothed-particle hydrodynamics (SPH)
simulations. The method was applied to modeling formation of main-belt families
during the cometary bombardment (either early or late, ${\sim}\,3.85\,{\rm Gy}$
ago). If asteroids were bombarded by comets, as predicted by the Nice model,
hundreds of asteroid families (catastrophic disruptions of diameter $D \ge
100\,{\rm km}$ bodies) should have been created, but the observed number is
only 20. Therefore we computed a standard set of 125 simulations of collisions
between representative $D = 100\,{\rm km}$ asteroids and high-speed icy
projectiles (comets). According to our results, the largest remnant mass
$M_{\rm lr}$ is similar as in low-speed collisions, due to appropriate scaling
with the effective strength $Q_{\rm eff}$, but the largest fragment mass
$M_{\rm lf}$ exhibits systematic differences - it is typically smaller for
craterings and bigger for super-catastrophic events. This trend does not,
however, explain the non-existence of old families. The respective parametric
relations can be used in other statistical (Monte-Carlo) models to better
understand collisions between asteroidal and cometary populations.
