NOO inclinations intersected the comet evolution path of its inclination. The longitudes of the perihelia of the MON attain the same values as the nominal cometary orbit in the recent centuries and then disperse. On the other hand, the longitudes of the perihelia of the NOO remain much longer along the evolved nominal orbit of the comet and disperse slowly after thousands of years, which could support the younger age of MON as well. A similar feature is visible for the perihelion distance of both showers. Currently the perihelion distance of MON fits well with the current orbit of the comet but gets more dispersed around 500 B.C. The perihelion distance of NOO is slightly different during the last 2000 years but generally intercepts the perihelion distance of the comet earlier than 1000 B.C. The eccentricity of MON is dispersed much more in the past than in the case of NOO. The heliocentric distance of the ascending node of MON lies close to the current ascending node of the comet but disperses fast in the past. This distance is currently lower for NOO but could be explained by the orbital evolution (Figure 11). These implications of the orbital evolution suggest 