Table 1
Summary of important model parameters used in each step of the procedure.
| Symbol | Quantity | two-pop-py | MCMax | ProDiMo |
|---|---|---|---|---|
| R* | Stellar radius | 2.086 R⊙ | 2.086 R⊙ | |
| M* | Stellar mass | 0.70 M⊙ | 0.70 M⊙ | 0.70 M⊙ |
| Mdisk∕M* | Initial disk mass | 0.1 | ||
| Rtaper | Taper radius | 100 AU | 100 AU | |
| γvisc | Viscosity exponent | 1 | ||
| Ngrains | Number of dust grains | 150 | 150 | |
| amin | Minimum dust grain size | 10−5 cm | 10−5 cm | |
| amax | Maximum dust grain size | 1.9 × 102 cm | ||
| fvac | Dust grain porosity (vacuum fraction) | 0.25 | ||
| fmax | Maximum hollow volume ratio | 0.8 | ||
| tmax | Final timestep | 107 yr | ||
| αturb | Turbulence | 10−3 | 10−3 | |
| Rin | Inner radius | 0.06835 AU | 0.07 AU | |
| Rout | Outer radius | 2000 AU | 600 AU | |
| g∕d | Initial gas-to-dust ratio | 100 | ||
| T* | Stellar surface temperature | 4000 K | 4000 K | 4000 K |
| Nrad | Number of radial grid points | 240 | 500 | 240 |
| Nθ | Number of azimuthal grid points | 150 | ||
| NZ | Number of vertical grid points | 160 | ||
| Ninner | Number of radial points near inner rim | 100 | ||
| gasevol | Gas evolution | true | ||
| D | Distance of the disk | 140 AU | 140 AU | |
| i | Inclination of the disk | 45° | 45° | |
| χISM | Interstellar radiation field (Draine 1978) | 1 | 1 | |
| H0 | Gas scale height at 1 AU | 0.05012 AU | ||
| β | Flaring exponent | 1.15 | ||
| scset | Self-consistent dust settling | true | ||
| L* | Stellar luminosity | 1.0 L⊙ | ||
| fPAH | PAH abundance (relative to ISM) | 10−4 | ||
| fUV∕L* | UV excess | 0.01 | ||
| pUV | UV power-law exponent | 1.3 | ||
| ζCR | Cosmic ray H2 ionization rate | 1.7 × 10−17 s−1 | ||
| LX-ray | X-ray luminosity | 1030 erg s−1 | ||
Notes.Some parameters, for example the disk mass, are important for two-pop-py, MCMax, and ProDiMo. These parameters are not listed for the subsequent codes because their effects are embedded in the data passed between the codes. The only parameter in this table that is passed through to FLiTs is the disk inclination. Of the two-pop-py parameters in this table, the disk mass and gas-to-dust ratio are only valid for the initial state of the disk. The other parameters in this table are constant in time. The value Ngrains is the number of grain sizes used for the two-pop-py reconstruction of the grain size distribution. The dust is a distribution of hollow spheres, where the maximum fractional volume filled by the central void is 0.8 (Min et al. 2005, 2016). The dust grain mixture in MCMax is 60% amorphous Mg0.7 Fe0.3 Si O3 silicates (Dorschner et al. 1995), 15% amorphous carbon (Zubko et al. 1996), and 25% vacuum. The viscosity helps define the surface density Σg(r), where 
with a characteristic radius rc = 60 AU (Birnstiel et al. 2012).
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