Table 4
Influence of the K2 orbit uncertainties on the elements at the previous perihelion.
| solution | a8 | a9 | a6 | c5 | b5 |
|---|---|---|---|---|---|
| K2-prev-A: | |||||
| qprev (au) | 2.751–3.999–8.755 | 8.449–12.00–18.13 | 15.47–16.87–18.48 | 9.815–11.24–13.06 | 5.691 ± 0.101 |
| 1/aprev (10−6au−1) | 48.26 ± 7.93 | 35.48 ± 2.33 | 33.01 ± 0.46 | 35.96 ± 0.91 | 42.77 ± 0.23 |
| Pprev (Myr) | 2.98 | 4.73 | 5.27 | 4.63 | 3.57 |
| K2-prev-B: | |||||
| qprev (au) | 1.790–108.5–380.2 | 373.5–441.6–490.0 | 474.9–483.7–491.5 | 406.1–431.1–454.1 | 257.4 ± 6.3 |
| 1/aprev (10−6 au−1) | 37.84–49.79–58.31 | 34.88 ± 2.61 | 32.12 ± 0.50 | 35.41 ± 1.02 | 43.19 ± 0.27 |
| Pprev (Myr) | 2.84 | 4.85 | 5.49 | 4.74 | 3.52 |
Notes. For each orbital solution, we use 5001 clones of K2 orbit. Simulation K2-prev-A describes the results obtained when all stellar perturbations were excluded, while K2-prev-B reflects the results obtained from the full dynamical model with 232 potential stellar perturbers included, using their nominal tracks. In both variants, the full Galactic potential was taken into account.
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