A. Sekhar and D. J. Asher

Saturnian mean motion resonances in meteoroid streams

Figure 4. (a) Ecliptic plane crossings; and (b) distribution of heliocentric distances, for sets of 1:3 Saturnian MMR and non-resonant Orionid particles in 450 A.D. Both sets of particles evolved dynamically for 2 kyr but the dense clustering of resonant meteoroids contrasts with the large dispersion of non-resonant particles.


Many previous works have shown the relevance and dynamics of Jovian mean motion resonances (MMR) in various meteoroid streams. These resonant swarms are known to have produced spectacular meteor displays in the past. In this work we investigate whether any MMR due to Saturn are feasible, and subsequently check whether such effects are strong enough to trap meteoroids so as to cause enhanced meteor phenomena on Earth. Extensive numerical simulations are done on two major meteoroid streams, which are known to exhibit exterior Jovian resonances. The roles of the 1:6 and 5:14 Jovian MMR have already been studied in the Orionids and Leonids respectively. Now we find strong evidence of 1:3 and 8:9 Saturnian MMR in Orionids and Leonids respectively. The presence of compact dust trails in real space due to these two Saturnian resonances is confirmed from our calculations.

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Last Revised: 2013 May 17th