Table 3
Model parameters, and values for the reference model.
| Quantity | Symbol | Value |
|
|
||
| Stellar mass | M ⋆ | 0.7 M⊙ |
| Effective temperature | T ⋆ | 4000 K |
| Stellar luminosity | L ⋆ | 1 L⊙ |
| UV excess | f UV | 0.01 |
| UV powerlaw index | p UV | 1.3 |
| X-ray luminosity | L X | 1030 erg/s |
| X-ray emission temperature | T X,fit | 2 × 107 K |
|
|
||
| Strength of interstellar UV | χ ISM | 1 |
| Strength of interstellar IR |
|
0 |
| Cosmic ray H2 ionisation rate | ζ CR | 1.7 × 10-17 s-1 |
|
|
||
| Disk massa | M disk | 0.01 M⊙ |
| Dust/gas mass ratioa | δ | 0.01 |
| Inner disk radius | R in | 0.07 AU |
| Tapering-off radius | R tap | 100 AU |
| Column density power index | ϵ | 1 |
| Reference scale height | Hg(100 AU) | 10 AU |
| Flaring power index | β | 1.15 |
|
|
||
| Minimum dust particle radius | a min | 0.05 μm |
| Maximum dust particle radius | a max | 3 mm |
| Dust size dist. power index | a pow | 3.5 |
| Turbulent mixing parameter | α settle | 0.01 |
| Max. hollow volume ratio |
|
80% |
| Dust composition | Mg0.7Fe0.3SiO3 | 60% |
| (volume fractions) | amorph. carbon | 15% |
| porosity | 25% | |
|
|
||
| PAH abundance rel. to ISM | f PAH | 0.01 |
| Chemical heating efficiency | γ chem | 0.2 |
|
|
||
| Distance | d | 140 pc |
| Disk inclination | i | 45° |
Notes.
The total disk dust mass Mdust and the dust/gas ratio δ are the primary parameters in this paper, whereas the total disk mass Mdisk = Mgas is derived from Mdust and δ. Changing Mdisk means to change Mdust as well, by the same factor, whereas changing δ (or the inverse called “gas/dust” later) means to change Mdisk, but not to change Mdust. The chemical heating efficiency γchem is an efficiency by which exothermal chemical reactions are assumed to heat the gas, see (Woitke et al. 2011, see Appendix A.8 therein) for details.
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