Table D.1
Model parameters and values for the reference model.
Quantity | Symbol | Value |
---|---|---|
Stellar mass | M⋆ | 0.7, 2.3 M⊙ |
Effective temperature | T⋆ | 4000, 8600 K |
Stellar luminosity | L⋆ | 1, 32 L⊙ |
UV excess | fUV | 0.01 |
UV power-law index | pUV | 1.3 |
X-ray luminosity | LX | 1030 erg/s |
X-ray emission temperature | TX,fit | 2 × 107 K |
Strength of interstellar UV | χISM | 1 |
Strength of interstellar IR | ![]() |
0 |
Cosmic ray H2 ionization rate | ζCR | |
Disk mass (1) | Mdisk | 0.01 M⊙ |
Dust/gas mass ratio (1) | δ | 0.01 |
Inner disk radius | rin | 0.07 AU |
Tapering-off radius | rtap | 100 AU |
Column density power index | ɛ | 1 |
Rreference scale height | Hg(100 AU) | 10 AU |
Flaring power index | β | 1.15 |
Minimum dust particle radius | amin | 0.05 μm |
Maximum dust particle radius | amax | 3 mm |
Dust size dist. power index | apow | 3.5 |
Turbulent mixing parameter | αsettle | 0.01 |
Max. hollow volume ratio | ![]() |
80% |
Dust composition | Mg0.7Fe0.3SiO3 | 60% |
(volume fractions) | amorph. carbon porosity | 15% |
PAH abundance rel. to ISM | fPAH | 0.01 |
Chemical heating efficiency | γchem | 0.2 |
Distance | d | 140 pc |
Disk inclination | i | 45° |
12C/13C | 70 (150) (2) | |
18O/16O | 540 | |
Thermal over magnetic | βmid | 102–106 |
in the midplane |
Notes. The meaning of the symbols is explained in Woitke et al. (2009, 2016). (1) The chemical heating efficiency γchem is the efficiency by which exothermic chemical reactions are assumed to heat the gas. A detailed discussion on the disk parameters and their effects on the disk thermal and chemical structure can be found in Woitke et al. (2016). (2) 70 is the adopted standard value (Henkel et al. 1994; Wilson 1999). The choice of 100 corresponds to an average value between the observed ratios by Smith et al. (2015) towards YSOs.
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