Examination of the transportation abilities of the 3:1 MMR with Jupiter II

Resonances play a significant role in the transport of bodies throughout the Solar System and, therefore, also in the transport to the NEO (Near-Earth Object) region.

Our last presentations at EPSC conferences were dedicated to the transportation abilities of the 5:2 and 3:1 MMRs (Mean Motion Resonances) with Jupiter [1, 2]. It was interesting to find that the 5:2 MMR may not be as inefficient in transport into the NEO region as we thought, compared to the 3:1 MMR. However, our integrations did not include non-gravitational effects to be consistent with previous studies. To select initial conditions for the simulations, we used short-term FLI (Fast Lyapunov Indicator [3]) maps to differentiate between stable and unstable orbits. This time, we decided to include non-gravitational effects, specifically the Yarkovsky effect, because we are also interested in potentially hazardous objects. Other non-gravitational effects (e.g., Poynting-Robertson effect) are effective mainly for dust particles.

We study the 3:1 MMR with Jupiter again to determine how significant the difference will be after adding the Yarkovsky effect to the integrations. We use an implementation of the Yarkovsky effect available within REBOUNDx [4]. We plan to repeat our simulations for 10 Myr with the same initial conditions as previously; however, these particles will no longer be massless. We started with generally used values, such as 0.15 for albedo and 2.5 g/cm³ for mean density. We plan to take several particle radii into account and also to consider migration inwards as well as outwards. For each combination of these values, we will integrate the whole set of 10080 particles and track their orbital evolution. Later, we want to try also other values for albedo and mean density. As in previous works, we are interested in transport into the NEO region, final states, migration toward the Sun, close encounters and collisions with planets or the Sun, potentially hazardous orbits, etc.

At EPSC 2026 in the Hague, we will present our preliminary results.

 

Acknowledgement:

This work was supported by the PostdokGrant APD0197 and by the VEGA - Slovak Scientific Grant Agency, grant No. 2/0041/26.

 

References:

[1] Kováčová, M.: Re-examination of the transportation abilities of the 5:2 MMR with Jupiter, Europlanet Science Congress 2024, Berlin, Germany, 8–13 Sep 2024, EPSC2024-565, https://doi.org/10.5194/epsc2024-565, 2024.

[2] Kováčová, M.: Examination of the transportation abilities of the 3:1 MMR with Jupiter, EPSC-DPS Joint Meeting 2025, Helsinki, Finland, 7–12 Sep 2025, EPSC-DPS2025-355, https://doi.org/10.5194/epsc-dps2025-355, 2025.

[3] Skokos C., Gottwald G. & Laskar J., 2016, Chaos detection and predictability (Chapter 2)

[4] REBOUNDx (https://reboundx.readthedocs.io/en/latest/)