escaping only from the Sun-facing hemisphere with the Gaussian distribution of velocities with the center on the subsolar point, the maximum ejection velocity might range from 5m/s [@imp01] to 112m/s [@crifo; @ma02]. The escape velocity of the meteoroid particle changes its orbital elements so that we may calculate according to @pec97.

On the other hand, if we know the orbital elements of the comet (before the ejection of the meteoroid) and the meteoroid after the ejection (assuming that the observed meteoroid escaped the comet recently and did not undergo rapid orbital changes due to gravitational and non-gravitational perturbations), we may directly derive the ejection velocities from equations by @pec97 as a low estimate. The ejection velocity affects, at most, the semimajor axis. In the perihelion, the semimajor axis change is ruled by the transversal component of the velocity vector $\Delta v_{t}$. The range of ejection velocities derived according to mean, the peak and minimum-maximum values of the semimajor axis (Figure 2) of each meteor shower, in comparison with the range of semimajor axes of the cometary clones, integrated 2000yr to the past is presented in Table 5. The mean and peak values of the transversal ejection velocity components are in 