Table 1
Overview of the simulations.
| Model | vr,0 (km s-1) | vφ,0 (km s-1) | φ0 (deg) | Expected periastron (AU) | Actual periastron (AU) | Fragment ejected? |
|
|
||||||
| P1 | –1.8 | 0.5 | 90 | 473 | 412 | yes |
| P2 | –2.1 | 0.7 | 90 | 704 | 659 | yes |
| P3 | –1.9 | 0.6 | 90 | 606 | 556 | yes |
| P4 | –1.7 | 0.45 | 90 | 410 | 338 | yes (2) |
| P5 | –1.8 | 0.5 | 180 | 473 | 391 | yes (2) |
| P6 | –1.8 | 0.5 | 270 | 473 | 467 | yes (2) |
|
|
||||||
| R1 | –1.8 | –0.5 | 90 | 473 | 466 | yes |
| R2 | –2.1 | –0.7 | 90 | 704 | 700 | no |
| R3 | –1.9 | –0.6 | 90 | 606 | 601 | no |
| R4 | –1.7 | –0.45 | 90 | 410 | 397 | no |
| R5 | –1.8 | –0.5 | 270 | 473 | 423 | no |
| R6 | –1.8 | –0.5 | 0 | 473 | 384 | no |
Notes. Columns show, from left to right, the model identifier (the names of prograde models start with P, the ones of retrograde models with R), radial and azimuthal components of the initial velocity of the intruder vr,0 and vφ,0, the initial azimuthal position of the intruder φ0, expected (calculated analytically treating the disk-star system as a point mass) and actual periastron radius and whether fragments have been ejected during the simulation.
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