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Table 6

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 fUV 0.01
UV powerlaw index pUV 1.3
X-ray luminosity LX 1030 erg s−1
X-ray emission temperature TX,fit 2 × 107 K

Strength of interstellar UV χISM 1
Strength of interstellar IR 0
Cosmic ray H2 ionisation rate ζCR 1.7 × 10−17 s−1

Disk mass Mdisk 0.01 M
Dust/gas mass ratio δ 0.01
Inner disk radius Rin 0.07 AU
Tapering-off radius Rtap 100 AU
Column density power index ɛ 1
Reference 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 (1) Mg0.7 Fe0.3 SiO3 60%
(Volume fractions) amorph. carbon 15%
Porosity 25%

PAH abundance rel. to ISM fPAH 0.01
Chemical heating efficiency (2) γchem 0.2

Distance d 140 pc
Disk inclination i 45°

Photodesorption Yield 10−2–10−3
Number of chemisorbed layers Ncore,layer 500

Notes. (1) The dust composition and porosity best match protoplanetary disk observations of protoplanetary disks, although the porosity of the comet 67P/Churyumov-Gerasimenko is 75–85 per cent in volume (Herique et al. 2016). (2) The chemical heating efficiency γchem is an 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). The photodesorption yield depends on the species. Special rates are used for water ice (Westley et al. 1995; Öberg et al. 2009) and CO ice (Muñoz Caro et al. 2010). For the other ice species, a standard yield of 10−3 is assumed.

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