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Table 5.
PARSEC 1.2S and COLIBRI S_37 models of each component of MWC 166 A.
| Parameter | MWC 166 Aa | MWC 166 Ab |
|---|---|---|
| Mdyn [M⊙] | 12.19 ± 2.18 | 4.90 ± 0.52 |
| Age [yr] | 1.0 × 105 | |
| L [L⊙] |
 |
 |
| R [R⊙] |
 |
 |
| Teff [K] |
 |
 |
| log(g) |
 |
 |
| Age [yr] | 5.0 × 105 | |
| L [L⊙] |
 |
 |
| R [R⊙] |
 |
 |
| Teff [K] |
 |
 |
| log(g) | 4.27 ± 0.02 |
 |
| Age [yr] | 1.0 × 106 | |
| L [L⊙] |
 |
 |
| R [R⊙] |
 |
 |
| Teff [K] |
 |
 |
| log(g) | 4.25 ± 0.02 |
 |
| Age [yr] | 3.0 × 106 | |
| L [L⊙] |
 |
 |
| R [R⊙] |
 |
2.50 ± 0.16 |
| Teff [K] |
 |
 |
| log(g) | 4.20 ± 0.03 | 4.33 ± 0.01 |
| Age [yr] | 1.0 × 107 | |
| L [L⊙] |
 |
 |
| R [R⊙] |
 |
 |
| Teff [K] |
 |
 |
| log(g) |
 |
4.29 ± 0.02 |
Notes. Isochrones were selected at five representative ages including reasonable lower and upper bounds, with stellar parameters corresponding to the dynamical masses of each component. The isochrones assume solar metallicities and that the stars are coeval.
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