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Table D.2
Physical parameters and assumptions adopted for the dynamical analysis of the circumbinary disc around 3 Puppis.
| Quantity | Symbol (Unit) | Value | References |
|---|---|---|---|
| Gas to dust mass ratio | δ (...) | 100 | Kluska et al. (2018); Bujarrabal et al. (2013) |
| Dust mass | Mdust (M⊙) | 3.5 × 10−7 | from Table 1 |
| Gas mass | Mgas (M⊙) | 3.5 × 10−5 | = δ · Mdust |
| Dusty inner rim radius | Rrim (au) | 3.6 | from Table 1 |
| Temperature at the dusty inner rim | Trim (K) | 1 250 | from Table 1 |
| Mean molecular weight | μ (...) | 2.3 | Hayashi (1981), D’Alessio et al. (1998) |
| Mass of the 3 Puppis system | Mtot (M⊙) | 9.55 | = M* + Mc, derived from Table 1 |
| Sound speed | cs (ms−1) | 2116 | derived from Table D.1 Equation 2 |
| Kinematic viscosity parameter | α (...) | 10−2 | Hartmann (1998); Rafikov (2016) |
| Clump radial thickness | w (au) | 0.23 | = H(Rref), derived from Table D.1 Equation 5 |
| Clump angular width sector | ∆φ (°) | 30 | derived from M-band MYTHRA image |
| Density contrast amplitude | Γ (%) | 20 | derived from M-band MYTHRA image |
| Spiral pitch angle | ψ (°) | 15 | Ogilvie & Lubow (2002); Rafikov (2002); Dong et al. (2015) |
| Gaussian angular width | σφ (°) | 20 | Dong et al. (2015); Zhu et al. (2015) |
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