Speaker
Description
Maria Family is an old S-type asteroid family named after 170 Maria. Within the evolution, its members have separated with perturbation from 2.55 au distance to the Sun. There are two dynamical effects making them change their original orbits. One is mean-motion resonance (MMR), and the other is non-gravitational force, Yarkovsky effect. In this work we will investigate these two dynamical factors during Maria family's orbital evolution, analyzing how they become near-Earth asteroids. It's clear to see the distribution of members through Yarkovsky v-shape diagram and the existence of gap at 3:1 MMR and 8:3 MMR. We also analyze whether it's related to eccentricity or inclination during simulations, and the dynamical motion nearby both MMRs. We expect that we will find the truth of becoming near-Earth asteroids through 3:1 MMR and retrograde Yarkovsky drift.
| Participate the oral/poster presentation award competition | Yes |
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