Table 1
Cosmogonic models that make predictions of the population of refractory objects in the Oort cloud.
| Model | Main mechanisms | Particles’ size regime | Predicted population of refractory objects in the Oort cloud |
|---|---|---|---|
| Weissman & Levison (1997) | Gravitational perturbations of giant planets | Planetesimals | ~3–6% [1,10] ~0.25–0.5% [10] |
| Nice model [2,3,4] | Planetary migrations (planetesimal and planet-planet scattering), mean-motion orbital resonances | Planetesimals | ~0.001% [11] |
| The Grand Tack [5] | Planetary migrations (gas-driven), mean-motion orbital resonances | Planetesimals and planetary embryos | ~0.1–0.2% [10] ~1% [11] |
| Pebble accretion [6,7] | Gravity, gas drag | Pebbles | ~0.01% [10] |
| Depleted Disk model [8] | Gravitational perturbations of giant planets, secular resonances | Planetesimals and planetary embryos | ~0.25–0.5% [10] |
| Shannon et al. (2015) | Gravitational perturbations of giant planets and passing stars, galactic tides | Planetesimals | ~4% [9] ~0.05% [10] |
| The Static case [11] | Gravitational perturbations of giant planets and passing stars, galactic tides, dynamical and collisional evolution | Planetesimals | ~0.01–0.001% [11] |
| Portegies Zwart et al. (2021) | Gravitational perturbations of giant planets and stars from the cluster, galactic tides, mean-motion orbital resonances | Planetesimals | Neglectable [12] |
Notes. Table provides model mechanisms and sizes of considered particles. In the last column, several estimates for the same model according to different authors are provided (if available), the latest estimates are the most relevant. [1] Weissman & Levison (1997); [2] Gomes et al. (2005); [3] Morbidelli et al. (2005); [4] Tsiganis et al. (2005); [5] Walsh et al. (2011); [6] Lambrechts & Johansen (2012); [7] Levison et al. (2015); [8] Izidoro et al. (2013); [9] Shannon et al. (2015); [10] Meech et al. (2016); [11] Shannon et al. (2019); [12] Portegies Zwart et al. (2021).
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