Table 2
Analytical model for stellar encounters for an encounter distance of 1 pc.
| S.T |  (Myr−1) |
 (km s−1) |
 |
|---|---|---|---|
| B0V | 0.005 | 8.77e-03 | 4.742 |
| A0V | 0.023 | 1.005e-03 | 22.973 |
| A5V | 0.032 | 6.716e-04 | 32.007 |
| F0V | 0.072 | 4.701e-04 | 71.536 |
| F5V | 0.212 | 3.161e-04 | 211.527 |
| G0V | 0.258 | 2.485e-04 | 257.608 |
| G5V | 0.276 | 2.151e-04 | 275.696 |
| K0V | 0.576 | 2.195e-04 | 576.229 |
| K5V | 0.918 | 1.348e-04 | 917.675 |
| M0V | 1.401 | 1.108e-04 | 1400.844 |
| M5V | 6.915 | 3.293e-05 | 6915.189 |
| WD | 1.263 | 8.143e-05 | 1262.623 |
| Giants | 0.623 | 4.617e-04 | 622.765 |
Notes. Thespectral type is shown in Col. 1, the frequency of the stellar encounters is shown in Col. 2, the change in the velocity of a comet due to an interaction with a star is shown in Col. 3, and the total number of stars entering a sphere of radius 1 pc around the Sun–comet system over a time interval of 1 Gyr is shown in Col. 4.
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