altered in order to put ascending node close to 1AU at the present day.[]{data-label="F8"}](fig8-b.eps){width="8.0cm"}

![image](fig9-a.eps){width="7.0cm"} ![image](fig9-q.eps){width="7.0cm"}

![image](fig9-i.eps){width="7.0cm"} ![image](fig9-lonperi.eps){width="7.0cm"}

\[F9\]

![image](fig10-Ma.eps){width="7.0cm"} ![image](fig10-Na.eps){width="7.0cm"}

![image](fig10-Me.eps){width="7.0cm"} ![image](fig10-Ne.eps){width="7.0cm"}

![image](fig10-Mq.eps){width="7.0cm"} ![image](fig10-Nq.eps){width="7.0cm"}

![image](fig10-Mi.eps){width="7.0cm"} ![image](fig10-Ni.eps){width="7.0cm"}

\[F10\]

![image](fig10-Mlonperi.eps){width="7.0cm"} ![image](fig10-Nlonperi.eps){width="7.0cm"}

![image](fig10-Masc.eps){width="7.0cm"} ![image](fig10-Nasc.eps){width="7.0cm"}

![image](fig10-Mdesc.eps){width="7.0cm"} ![image](fig10-Ndesc.eps){width="7.0cm"}

\[F11\]

As mentioned previously, the orbit of the parent comet was determined with a low precision. In our study, we set out to calculate the orbital evolution of nominal and cloned orbits of the parent comet. We created 100 clones within the 0.8yr uncertainty of the orbital period [@ask32], with fixed perihelion distance and altered semimajor axis and eccentricity accordingly. We could not modify other orbital elements because their uncertainties are unknown. Another set of 100 clones was made in order to create orbits with the heliocentric distance of ascending node close to 1AU while neither nominal orbit nor first 100 clones have the ascending node close enough to the orbit of the Earth to create an observed meteor shower. In this case, the eccentricity, the semimajor axis and the perihelion distance were altered. The beginning of the integration was set at the epoch of the perihelion passage of C/1917 F1 Mellish (JD 2421334.0, Eq. 2000.0). The multistep Adams-Bashforth-Moulton type up to 12th order numerical integrator, 