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Table 4
Model ability to reproduce observational characteristics.
| Simulation 19 | Simulation 20 | |
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| Primary’s stellar distribution | yes | yes |
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| Secondary’s stellar distribution | too distorted | OK with different projection (20°) |
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| Distorted Hi envelop | no | no |
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| Prominent Hi and CO gas bridge | yes | yes |
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| CO bridge emission offset w.r.t. Hi to the south | yes | yes |
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| Symmetric gas velocity fields in the disks | no | yes |
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| Isovelocity contours parallel to the bridge | yes | yes |
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| Hi double-line profile in the bridge region | yes | yes |
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| CO emission only associated with the high-velocity line | yes | yes |
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| Large gas linewidths in the bridge region | ||
| (100−200 km s-1) | yes | yes |
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| Small separation between the double lines | ||
| (~330 km s-1) | yes | no |
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| High field strength of the bridge regular | ||
| magnetic field | yes | yes |
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| Projected B field vectors parallel to the bridge | with offset of ~ 30° | yes |
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| Polarized intensity maximum offset to the south | ||
| of the bridge | no | yes |
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| Gas bridge strong in total power radio | ||
| continuum emission | due to high turbulent velocity | due to high turbulent velocity |
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