Table 1.
Avalanche exponents for the different setups.
| τt | τ | α1 | α | αcoll | |
|---|---|---|---|---|---|
| (1) | −1.46 ± 0.04 | −1.24 ± 0.03 | 1.45–2.25 | 1.92 ± 0.08 | ∼2 |
| (2) | −1.630 ± 0.013 | −1.327 ± 0.010 | 1.49–1.82 | 1.93 ± 0.06 | 1.92 ± 0.02 |
| (3) | −1.636 ± 0.021 | −1.327 ± 0.010 | 1.89 ± 0.02 | 1.94 ± 0.06 | 1.92 ± 0.02 |
| (4) | −1.650 ± 0.015 | −1.385 ± 0.010 | 1.27–1.98 | 1.69 ± 0.06 | 2.15 ± 0.03 |
Notes. Setup 1: Baseline cellular automaton, following Mineshige et al. (1994a,b). Setup 2: Cellular automaton with a link between gas accretion and wind emission, as in MCDW models. Setup 3: As in setup 2, but with an Eddington-like limit on the mass-accretion rate at the outer radius. Setup 4: As in setup 1, but with a threshold on disk luminosity above which the accretion is halted. α1 is the best linear regression to the full ⟨S⟩(T) distribution for setup 3, while for setups 1, 2, and 4 the two values refer to the best linear regression for T < 10 and T > 10.
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