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Table 3
Summary of the main features of relevant SiO maser pumping models currently available and their predicted relative spatial offsets between the three transitions.
| Model | Type of system | Main feature | v = 2, J = 1−0 with respect to v = 1, J = 1−0 | v = 1, J = 2−1 with respect to v = 1, J = 1−0 |
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| Humphreys et al. (2002) | single evolved star | hydrodynamic shocks | ~ 0% (co-spatial) | ~ 2% further away |
| Soria-Ruiz et al. (2004) | single evolved star | overlaps with H2O absorption lines | ~ 0% (co-spatial) | ~ 50% further away |
| Gray et al. (2009) | single evolved star | hot dense dust | ~ 0% (co-spatial) | ~ 25% further away |
| Goddi et al. (2009) | single YSO | radiative transfer (LVG) | slightly closer in | ~ 0% (co-spatial) |
| Gray et al. (in prep.) | binary YSO | full hydrodynamic solution for binary | ~ 3% closer in | ~ 20% further away |
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