Table 4
Main fixed parameters of the disk model.
| Quantity | Symbol | Value |
|
|
||
| stellar mass | M ∗ | 0.7 M⊙ |
| stellar effective temp. | T ∗ | 4000 K |
| stellar luminosity | L ∗ | 1.0 L⊙ |
| FUV excess | L FUV / L ∗ | 0.01 |
| FUV power law index | p UV | 1.3 |
|
|
||
| strength of interst. FUVa | χ ISM | 1 |
|
|
||
| disk gas mass | M disk | 0.01 M⊙ |
| dust/gas mass ratio | d / g | 0.01 |
| inner disk radius | R in | 0.07 au |
| tapering-off radius | R tap | 100 au |
| column density power ind. | γ | 1.0 |
| reference scale height | H(100au) | 10 au |
| flaring power index | β | 1.15 |
|
|
||
| min. dust particle radius | a min | 0.05 μm |
| max. dust particle radius | a max | 3 mm |
| dust size dist. power index | a pow | 3.5 |
| turbulent mixing param. | α settle | 10-2 |
| max. hollow volume ratiob | V hollow,max | 0.8 |
| dust composition | Mg0.7Fe0.3SiO3 | 60% |
| (volume fractions) | amorph. carbon | 15% |
| porosity | 25% | |
Notes. If not noted otherwise, these parameters are kept fixed for all our models presented in this work. For more details on the parameter definitions see Woitke et al. (2009, 2011, 2016).
χISM is given in units of the Draine field (Draine & Bertoldi 1996; Woitke et al. 2009).
We use distributed hollow spheres for the dust opacity calculations (Min et al. 2005, 2016).
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