Table A.5
α and St assumed in the models, derived based on fragmentation limited dust sizes, or to explain accretion.
| Name | Domain (au) | αz,MCFOST (−) | StMCFOST (×10−3) | αfrag (×10−4) | Stfrag (×10−3) | αacc (×10−4) |
|---|---|---|---|---|---|---|
| AA Tau | 43 − 93 | ≤ 2e-2 | 35.0 | ≤ 10.3 | ≥ 5.1 | − |
| 93 − 160 | ≤ 2e-3 | 85.0 | ≤ 3.2 | ≥ 25.6 | − | |
| AS209 | 39 − 97 | ≤ 2e-3 | 10.6 | ≤ 11.4 | ≥ 5.1 | 203.3 |
| 97 − 141 | ≤ 2e-4 | 19.9 | ≤ 4.0 | ≥ 19.8 | 203.3 | |
| CI Tau | 40 − 130 | ≤ 2e-2 | 14.9 | ≤ 34.7 | ≥ 2.2 | − |
| 130 − 234 | ≤ 2e-1 | 61.4 | ≤ 51.7 | ≥ 2.2 | − | |
| DL Tau | 46 − 78 | ≤ 2e-3 | 8.3 | ≤ 17.4 | ≥ 4.4 | − |
| DoAr25 | 69 − 86 | ≥ 2e-4 | 7.2 | ≥ 3.3 | ≤ 22.9 | − |
| 86 − 165 | ≤ 2e-3 | 11.4 | ≤ 13.6 | ≥ 7.4 | − | |
| DS Tau | 55 − 85 | ≤ 2e-3 | 18.5 | ≤ 8.9 | ≥ 9.7 | − |
| Elias24 | 37 − 123 | ≤ 2e-3 | 10.4 | ≤ 6.5 | ≥ 7.0 | − |
| GM Aur | 40 − 125 | ≤ 2e-3 | 9.9 | ≤ 10.2 | ≥ 5.4 | 28.5 |
| GO Tau | 73 − 150 | ≤ 2e-2 | 36.0 | ≤ 14.9 | ≥ 8.0 | − |
| GW Lup | 62 − 141 | ≤ 2e-3 | 39.2 | ≤ 4.1 | ≥ 20.4 | 8.8 |
| Haro 6-5B | 110 − 190 | ≤ 2e-2 | 37.2 | ≤ 10.5 | ≥ 7.0 | − |
| HD142666 | 11 − 30 | ≥ 2e-4 | 6.1 | ≥ 1.7 | ≤ 11.1 | ≤ 5.1 |
| 40 − 60 | ≤ 2e-3 | 11.2 | ≤ 11.2 | ≥ 3.3 | ≤ 5.1 | |
| HD163296 | 49 − 85 | 2e-4 − 2e-1 | 18.8 | 16.4 | 2.0 | 64.4 |
| 85 − 155 | ≤ 2e-4 | 31.7 | ≤ 1.9 | 26.6 | 64.4 | |
| HL Tau | 61 − 150 | ≤ 2e-2 | 10.5 | ≤ 8.3 | ≥ 3.1 | − |
| ISO-Oph 17 | 26 − 46 | ≤ 2e-1 | 10.3 | ≤ 58.4 | ≥ 0.7 | − |
| J1608 | 60 − 82 | ≤ 2e-3 | 55.7 | ≤ 2.2 | ≥ 9.0 | − |
| J1610 | 29 − 78 | ≤ 2e-2 | 31.0 | ≤ 10.3 | ≥ 5.4 | − |
| LkCa 15 | 47 − 89 | ≥ 2e-1 | 35.3 | ≥ 19.8 | ≤ 1.9 | 3.0 |
| 89 − 200 | ≤ 2e-2 | 35.7 | ≤ 14.5 | ≥ 5.3 | 3.0 | |
| MYLup | 40 − 100 | ≤ 2e-3 | 4.2 | ≤ 22.1 | ≥ 3.5 | − |
| Oph163131 | 107 − 150 | ≤ 2e-3 | 87.2 | ≤ 3.0 | ≥ 17.0 | − |
| PDS70 | 50 − 105 | ≤ 2e-3 | 24.6 | ≤ 4.8 | ≥ 10.5 | − |
| RY Tau | 28 − 90 | ≤ 2e-3 | 3.7 | ≤ 11.3 | ≥ 3.2 | − |
| V1094Sco | 107 − 164 | ≥ 2e-1 | 39.2 | ≥ 26.2 | ≤ 3.6 | 31.4 |
| 201 − 280 | ≤ 2e-2 | 42.8 | ≤ 19.1 | ≥ 6.5 | 31.4 |
Notes. Leftmost columns, αz and Stokes numbers assumed in our mcfost modeling for a grain size aMCFOST indicated in Table A.2. The middle columns assume dust size is limited by fragmentation, with a fragmentation velocity of vfrag = 1 m s−1, using the most conservative values of ζ = αz/St from Table A.3 (see Sect. 6.1). The rightmost column show the estimated global accretion turbulence for disks discussed in Sect. 6.2. We note that the ratio αz,MCFOST/StMCFOST are slightly different from the values reported in Table A.3, possibly because the constraints on Hd,R actually originate from the contribution of several grain sizes instead of just that with the maximum opacity.
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