Table 3
Results after 4.6 Gyr of model simulations for different Galactic model.
| Quantity | BGS | BS | BG | Φ |
|
|
||||
| σU8 [km s-1] | 37.5 | 17.1 | ||
| σV8 [km s-1] | 18.9 | 7.7 | ||
| σW8 [km s-1] | 16.9 | 8.8 | 15.2 | 9.1 |
| σU8/σW8 | 2.21 | 1.88 | ||
| σUa [km s-1] | 58.0 | 47.9 | 36.1 | 13.5 |
| σVa [km s-1] | 38.6 | 35.2 | 14.8 | 7.7 |
| σWa [km s-1] | 19.8 | 10.9 | 18.1 | 10.1 |
| ⟨ δR ⟩ [pc] | 74 | -256 | 195 | 85 |
| σδR [pc] | 1161 | 1020 | 946 | 409 |
| ⟨ R0 ⟩ [pc] | 7440 | 7700 | 7410 | 7830 |
| f400 [%] | 1.8 | 0.2 | 1.8 | <0.2 |
| S 400 | 2/6 | 1/1 | 1/9 | – |
Notes. BGS = bar+GMCs+spiral arms; BG = bar+GMCs, no spiral arms; BS = bar+spiral arms, no GMCs; Φ = Only overall Galactic potential. Dispersions in U, V and W velocities for model stars around the solar circle are given (indexed 8), as well as the corresponding dispersions for all the test particles (indexed a), means of the radial migration at the end of the simulation of all the stars from their starting points ⟨ δR ⟩, the dispersion of these measures in the radial direction σδR, the mean original Galactocentric radius of all stars around the solar circle ⟨ R0 ⟩ at 4.6 Gyr, the fraction of test particles ending with a distance greater than 400 pc from the Galactic plane f400, and the fraction S400 of such particles (ending above 400 pc) that would survive were they clusters. The fractions given suffer from small number statistics.
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