Table 3.
Results from the simulations.
| Model | v∞ | vRL, 1 | v∞/vorb | η | β | βBHL | (ȧ/a)bin | (ȧ/a)dyn | Accretion disk |
|---|---|---|---|---|---|---|---|---|---|
| – | km s−1 | km s−1 | – | – | – | – | yr−1 | yr−1 | – |
| Q1a5v1 | 6.0 | 2.1 | 0.291 | 0.610 | 0.298 | 0.571 | −8.18 × 10−6 | −9.11 × 10−6 | Yes |
| Q1a5v5 | 10.9 | 7.3 | 0.526 | 0.607 | 0.305 | 0.245 | −8.08 × 10−6 | −7.43 × 10−6 | Yes |
| Q1a5Ω | 15.1 | 12.5 | 0.733 | 0.557 | 0.212 | 0.135 | −7.17 × 10−6 | −3.73 × 10−6 | Yes |
| Q1a5 | 15.1 | 12.5 | 0.732 | 0.575 | 0.223 | 0.135 | −7.79 × 10−6 | −4.86 × 10−6 | Yes |
| Q1a10 | 15.1 | 14.1 | 1.035 | 0.376 | 0.099 | 0.061 | −6.58 × 10−8 | 9.91 × 10−7 | No |
| Q1a20 | 15.1 | 14.5 | 1.463 | 0.308 | 0.033 | 0.023 | 3.26 × 10−6 | 3.94 × 10−6 | No |
| Q13a5v1 | 6.0 | 2.1 | 0.311 | 0.548 | 0.323 | 0.386 | −1.23 × 10−5 | −1.12 × 10−5 | Yes |
| Q13a5v5 | 10.9 | 7.8 | 0.562 | 0.584 | 0.263 | 0.161 | −1.42 × 10−5 | −1.02 × 10−5 | Yes |
| Q13a5 | 15.1 | 13.0 | 0.782 | 0.363 | 0.125 | 0.086 | −3.93 × 10−6 | −7.03 × 10−7 | No |
| Q13a10 | 15.1 | 14.2 | 1.106 | 0.275 | 0.059 | 0.038 | 1.23 × 10−6 | 2.38 × 10−6 | No |
| Q13a20 | 15.1 | 14.5 | 1.565 | 0.220 | 0.016 | 0.014 | 4.80 × 10−6 | 5.24 × 10−6 | No |
| Q2a4v1Ω | 6.0 | 2.3 | 0.300 | 0.474 | 0.119 | 0.244 | −1.96 × 10−5 | −1.61 × 10−5 | Yes |
| Q2a4v1 | 6.0 | 2.3 | 0.300 | 0.515 | 0.263 | 0.244 | −2.32 × 10−5 | −1.45 × 10−5 | Yes |
| Q2a5v5Ω | 10.9 | 6.0 | 0.607 | 0.328 | 0.107 | 0.107 | −9.76 × 10−6 | −4.36 × 10−6 | Yes |
| Q2a5v5 | 10.9 | 6.0 | 0.607 | 0.381 | 0.128 | 0.085 | −1.36 × 10−5 | −5.61 × 10−6 | Yes |
| Q2a5Ω | 15.1 | 12.9 | 0.845 | 0.219 | 0.073 | 0.044 | −1.60 × 10−6 | 3.35 × 10−7 | No |
| Q2a5 | 15.1 | 12.9 | 0.845 | 0.214 | 0.067 | 0.044 | −1.08 × 10−6 | 1.91 × 10−7 | No |
| Q2a10 | 15.1 | 14.2 | 1.195 | 0.163 | 0.025 | 0.018 | 3.74 × 10−6 | 4.60 × 10−6 | No |
| Q2a20 | 15.1 | 14.5 | 1.689 | 0.131 | 0.007 | 0.007 | 6.63 × 10−6 | 6.95 × 10−6 | No |
| Q3a4v1 | 6.0 | 2.1 | 0.318 | 0.297 | 0.154 | 0.127 | −1.79 × 10−5 | −1.08 × 10−5 | No |
| Q3a5v5 | 10.9 | 8.6 | 0.644 | 0.160 | 0.052 | 0.043 | −2.96 × 10−6 | −2.35 × 10−6 | No |
| Q3a4 | 15.1 | 12.5 | 0.801 | 0.138 | 0.040 | 0.028 | −3.13 × 10−7 | 9.46 × 10−7 | No |
| Q3a5 | 15.1 | 13.2 | 0.896 | 0.127 | 0.031 | 0.022 | 1.32 × 10−6 | 2.51 × 10−6 | No |
| Q3a10 | 15.1 | 14.3 | 1.268 | 0.091 | 0.010 | 0.009 | 5.96 × 10−6 | 6.58 × 10−6 | No |
| Q3a20 | 15.1 | 14.5 | 1.793 | 0.073 | 0.003 | 0.003 | 8.17 × 10−6 | 8.48 × 10−6 | No |
| Q4a4v1 | 6.0 | 2.6 | 0.329 | 0.152 | 0.048 | 0.078 | −6.54 × 10−6 | −4.47 × 10−6 | No |
| Q4a5v5 | 10.9 | 8.7 | 0.665 | 0.110 | 0.032 | 0.026 | −1.20 × 10−6 | −5.00 × 10−7 | No |
| Q4a4 | 15.1 | 12.4 | 0.828 | 0.093 | 0.022 | 0.017 | 1.65 × 10−6 | 2.87 × 10−6 | No |
| Q4a5Ω | 15.1 | 13.4 | 0.925 | 0.084 | 0.019 | 0.013 | 3.02 × 10−6 | 4.39 × 10−6 | No |
| Q4a5 | 15.1 | 13.4 | 0.925 | 0.083 | 0.017 | 0.013 | 3.29 × 10−6 | 4.37 × 10−6 | No |
| Q4a10 | 15.1 | 14.4 | 1.308 | 0.058 | 0.005 | 0.005 | 7.27 × 10−6 | 7.67 × 10−6 | No |
Notes. v∞ is the average velocity of the wind at a distance 25Rd from a single star; vRL, 1 is the average velocity of the wind at the Roche lobe of the donor star taken assuming a single star undergoing mass loss via winds; v∞/vorb is the velocity ratio of the terminal velocity of the wind to the relative orbital velocity of the binary system; η is the average specific angular momentum-loss of the mass that crossed a boundary at 3a from the binary system in units of a2Ωbin as derived from Eq. (4); β is the average mass-accretion efficiency measured from the inflow in a shell at 0.4RL, 2; βBHL is the mass-accretion efficiency predicted by BHL determined from Eq. (10) with αBHL = 0.75; (ȧ/a)bin is the rate of change in the orbital separation of the binary system derived from Eq. (13); (ȧ/a)dyn is the rate of change in the orbital separation of the binary system derived dynamically from the simulation. For the corotating systems we cannot make a direct comparison for (ȧ/a)bin and (ȧ/a)dyn because in the first case the change in the orbital separation is computed from the change in the orbital angular momentum, whereas when measured dynamically the rate of change in a includes the change in angular momentum due to the spin of the donor star.
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