Table 1
Assumptions about disk shape, grain size, opacities, dust settling and PAHs in different thermo-chemical disk models.
| Reference | Model setup and disk shape | Radial range | Grain size | Dust opacities | Dust settling | PAHs |
| Semenov & Wiebe (2011), see Semenov et al. (2006) | adopted from D’Alessio et al. (1998), Tgas = Tdust | (10−700) AU | uniform 0.1μm | n.a. | well-mixed | n.a. |
| Gorti & Hollenbach (2008) | powerlaw Σ(r), modified CG97 | (0.5−200) AU | powerlaw, (0.005−50) μm | n.a. | well-mixed | reduced ISM abundance, PAHs in heating and chemistry |
| Dutrey et al. (2011), see also Semenov et al. (2010) | series of 1D vertical slabs, based on Hersant et al. (2009), Tgas = Tdust | (40−300) AU | uniform 0.1μm | n.a. | well-mixed | n.a. |
| Walsh et al. (2014), based on Nomura & Millar (2005) | Σ(r) from α-model, vertical hydrostatic equilibrium | (1−300) AU | MRN, details see (Nomura & Millar 2005) | mix of AS, graphite and water ice | well-mixed | n.a. |
| Du & Bergin (2014), based on Bethell & Bergin (2011) | powerlaw Σ(r) with self-similar tapered outer edge, parametric | (1−140) AU | 2 powerlaws: C1: (0.01−1) μm, C2: (1−100) μm | 7:3 mixture of AS and graphite | C1 well-mixed, C2 reduced H | reduced ISM abundance, for heating |
| Mathews et al. (2013), based on Qi et al. (2011) | powerlaw Σ(r) with self-similar tapered outer edge, modified parametric | complete disk | 2 powerlaws: C1: (0.005−0.25) μm, C2: 0.005 μm−1 mm | 3:2 mixture of AS and graphite | C1 well-mixed, C2 reduced H | n.a. |
| Akimkin et al. (2013) | viscous disk evolution, vertical hydrostatic equilibrium | (10−550) AU | dust evolution from initial MRN dist., (0.003−200) μm | AS | included in dust evolution | reduced ISM abundance, for heating |
| Bruderer (2013) | powerlaw Σ(r) with self-similar tapered outer edge, parametric | complete disk | 2 powerlaws: C1: (0.005−1) μm, C2: 0.005 μm−1 mm | mixture of AS and graphite | C1 well-mixed, C2 reduced H | reduced ISM abundance, in heating, chemistry and RT |
| Woitke et al. (2009) | powerlaw Σ(r), vertical hydrostatic equilibrium | (0.5−500) AU | powerlaw (0.1−10) μm | AS | well-mixed | reduced ISM abundance for heating |
| this work (more details in Sect. 3) | two zones, powerlaw Σ(r) with tapered outer edge, parametric | complete disk | powerlaw, 0.05 μm−3 mm | lab. silicates mixed with AC, DHS | Dubrulle et al. (1995), about 100 size bins | reduced ISM abundance, in heating, chemistry and RT |
Notes. CG97:two-layer model according to Chiang & Goldreich (1997); parametric:ρ(r,z) ∝ exp(−z2/ [2Hg(r)2]) with prescribed gas scale height Hg(r); modified parametric:parametric with more slowly declining tail into the upper regions, additional shape parameter for puffed-up inner rim; α-model:the surface density distribution Σ(r) is derived from the stellar mass, a constant disk mass accretion rate Ṁ, and the parametrised kinematic viscosity α (Shakura & Syunyaev 1973); complete disk:from inner rim (dust sublimation temperature) to some large distance where the column density becomes vanishingly small; RT:2D continuum radiative transfer; MRN:powerlaw size distribution f(a) ∝ a-3.5 between amin = 0.005 μm and amax = 0.25 μm (Mathis et al. 1977); AS:smoothed UV astronomical silicate (Draine & Lee 1984; Laor & Draine 1993); lab. silicates mixed with AC:optical properties from laboratory measurements of silicates and amorphous carbon, see Sect. 3.7 for deatils; DHS:distribution of hollow spheres (Min et al. 2005); reduced ISM abundance:PAH abundance lower than ISM standard (see Eq. (6)); dust evolution:detailed numerical simulations including growth, radial drift and settling according to Birnstiel et al. (2010).
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