SiO , 29 SiO and 30 SiO excitation : effects of infrared line overlaps

We have investigated the influence of several line overlaps between 28 SiO , 29 SiO and 30 SiO on maser emission from the envelopes of late-type stars using the Large Velocity Gradient radiative transfer formalism modified to account for overlaps. Our model includes: (i) 40 rotational levels for each of the v = 0 to 4 vibrational states and each isotopic species; (ii) collisions with molecular and atomic hydrogen; and (iii) radiative pumping by a shell of dust grains surrounding the SiO masing layers. We have shown that several line overlaps may play a role on the excitation of the 28 SiO v = 3, J = 1 → 0 maser, and on the anomalously weak v = 3, J = 2 → 1 emission. We suggest that 28 SiO maser emission in the v = 4, J = 5 → 4 line, the only one observed in this vibrational level, may also result from line overlaps. For 29 SiO , infrared line overlaps successfully explain observed maser emission in the v = 0, J = 5 → 4 and v = 1, 2, J = 6 → 5 lines. 30 SiO , v = 0, J = 2 → 1, and v = 0, J = 4 → 3 maser emissions could also result from line overlaps, and we find that several overlaps could explain the newly discovered maser line 30 SiO v = 1, J = 1 → 0. Finally, we make some predictions for new 28 SiO , 29 SiO and 30 SiO maser lines.