Table 3
Simulations of the Solar System in its birth star cluster using the LonelyPlanets approach (see Sect. 3.3.1).
| Star cluster simulation (see Sect. 3.3) | |
|---|---|
| Designation | Simulation B. |
| Simulations | Two-hundred simulations with 200 asteroids per star, and 24 simulations with 2000 asteroids per star in a cluster where stars interact with the asteroids. |
| Stars | Two-thousand stars with a Kroupa (2001) mass function between 0.08 and 100 M⊙ in R = 1 pc virialized Plummer sphere (Plummer 1911). No primordial binaries, no residual gas. |
| Planets | Four planets per star with circular orbits. Each star has the same planetary systems in a plane, but each planetary system has a different random orientation in space. In one model (extended), the planets Jupiter, Saturn, Uranus, and Neptune have initial semi-major axes 5.1, 9.5, 19.2, and 30.1 au, respectively. In the other model (compact), Jupiter, Saturn, Neptune, and Uranus have initial semi-major axes of 5.5, 8.1, 11.5, and 14.2 au. |
| Asteroids | In a disk between 40 au and 1000 au in the extended model and between 16 au and 400 au in the compact model. |
| Numerics | NBODY6++GPU (Wang et al. 2015) and REBOUND using IAS15 integrator (Rein & Spiegel 2015) coupled via the LonelyPlanets scheme (Cai et al. 2019) in AMUSE (Portegies Zwart & McMillan 2018). |
| Computer | Run on a GPU-equipped Little-Green-Machine-II (LGM-II) computer. |
| Duration | The simulations start with all stars on the zero-age main sequence with four planets in the adopted initial orbits. The calculation is continued for 100 Myr. |
Notes. The resulting orbital distribution of asteroids from the Sun-representative star is used in this work to further explore the evolution of the distribution of asteroids in the Oort cloud. These simulations do not lead to a reliable representation of abducted asteroids because the lonely planet approach does not allow exchange interactions.
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