Table 1
Parameters used in this study.
| Mdisk [M⊙ ] | rc [au ] | γ | vf [cm s−1 ] | Z0 | τf [torb] | αt | ε | LX [erg s−1] |
|---|---|---|---|---|---|---|---|---|
| 0.02 | 10 | 0.5 | 100 | 0.001 | 0 | 10−5 | 0.01 | 0 |
 |
 |
0.8 | 300 | 0.003 |  |
10−4 | 0.03 | 3 × 1028 |
| 0.10 | 35 |  |
 |
 |
600 |  |
 |
1029 |
| 50 | 1.2 | 0.02 | 1000 | 10−2 | 0.3 | 3 × 1029 | ||
| 100 | 1.5 | 0.03 | 1 | 1030 | ||||
 |
||||||||
| 0.10 | 20 | 1 | 200 | 0.0134 | 1600 | 3 × 10−4 | 0.05 | 3 × 1029 |
Notes. Standard values are marked in gray. Values for the second fiducial set are shown in bold. The columns list the disk mass Mdisk, characteristic radius rc, viscosity power-law index γ, which is also the power-law index of the column density of our initial condition for r ≪ rc, breakup speed of grains vf, initial dust-to-gas ratio Z0, trap formation time τf, turbulent viscosity parameter αt, planetesimal formation efficiency ε, and X-ray luminosity LX. For comparison, the disk mass of the MMSN is approximately 0.013M⊙. In a separate row, we highlight our most appropriate case, which includes a simple model for accretion heating that is not used in any other simulation.
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