Table 3
Subset of the models listed in Table 1, used to illustrate synthetic spectra, photometric properties, and their variability during the pulsation cycle (see Sect. 3.3 and related figures).
| Model | ΔMbol | Ṁ | uext | ΔV | |
|---|---|---|---|---|---|
| name | (mag) | (M⊙ yr−1) | (km s−1) | (mag) | |
| An315u3 / oli | 0.54 | 3 × 10−7 | 7 | 1.9 | SR |
| An114u3 / oli | 0.54 | 3 × 10−7 | 8 | 2.0 | SR |
| An315u4 / oli | 0.73 | 4 × 10−7 | 6 | 3.8 | M |
| An114u4 / oli | 0.73 | 5 × 10−7 | 9 | 4.3 | M |
| Bn315u3 / oli | 0.53 | 7 × 10−7 | 8 | 1.7 | SR |
| Bn114u3 / oli | 0.53 | 7 × 10−7 | 10 | 1.7 | SR |
| Bn315u4 / oli | 0.71 | 7 × 10−7 | 8 | 2.6 | M |
| Bn114u4 / oli | 0.71 | 8 × 10−7 | 10 | 2.5 | M |
| M2n315u6 / oli | 0.95 | 2 × 10−6 | 11 | 6.2 | M |
| M2n114u6 / oli | 0.95 | 2 × 10−6 | 16 | 5.6 | M |
Notes. Listed here are the bolometric amplitude ΔMbol (defined by input parameters), the resulting temporal means of the mass-loss rate Ṁ and the wind velocity uext, and the visual amplitude ΔV (derived a posteriori with COMA). According to definition, models with ΔV > 2.5 correspond to Mira variables, and smaller amplitudes correspond to semi-regulars (SRa or SRb). The model names are constructed in the following way: A, B, or M2 represents a combination of stellar parameters (see Sect. 3), the letter n followed by a 3-digit number stands for the seed particle abundance (n315 for nd ∕nH = 3 × 10−15, n114 for nd ∕nH = 1 × 10−14) and the letter u followed by a number (3, 4, 6) represents the velocity amplitude at the inner boundary (km s−1).
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