orbital element space. The mean orbits are presented in Table 2, in comparison with the mean orbits by other authors. Each orbital element was calculated as the median, with given standard deviation. The photometric mass was computed for each meteor according to @bet99 and its mean value for the showers is mentioned in Table 2. The orbits of the meteor showers are given in Figure 1. Figure 2 depicts selected orbital elements of both meteor showers. Figure 3 shows the $q-i$ phase space of individual meteors and nominal orbit of the comet C/1917 F1 Mellish.

The semimajor axes of both shower meteors seem to be much smaller than the nominal semimajor axis of the comet or even the range of semimajor axes derived from the 5000yr orbital evolution of cometary clones (the orbital evolution is described in chapter 3). The eccentricity, the perihelion distance and the inclination of MON are very close to the cometary orbit: the NOO meteors exhibit slightly lower but still high eccentricities, notably lower inclinations and lower perihelion distances. Generally, the orbits of MON and NOO are very similar. In $e$ and $q$ the values are the same within the standard deviation: a notable difference is 