Table D.1
DALI model parameters for the representative model for V883 Ori.
| Model parameter | Value | Ref. |
|---|---|---|
| Physical structure | ||
| Rsubl | 1 AU | |
| Rc | 75 AU | |
| Σc | 35 g cm-2 | |
| Mdisk | 0.25 M⊙ | |
| γ | 1 | |
| hc | 0.1 | |
| ψ | 0.25 | |
| Dust properties | ||
| χ | 0.2 | |
| fls | 0.9 | |
| Δgas∕dust | 100 | |
| Stellar spectrum(1) | ||
| Type | Outbursting | |
| L⋆+acc | 2.0(3), 6.0(3), 1.4(4) L⊙ | |
| LX | 1.4(30) erg s−1 | |
| Teff | 1(4) K | |
| Tacc | 1(4) K | |
| TX | 7(7) K | |
| ζcr | 5(–17) s-1 | |
| Stellar properties(2) | ||
| Ṁ | 5(−5) M⊙ yr−1 | |
| M⋆ | 1.3 M⊙ | (a) |
| R⋆ | 5.1 R⊙ | |
| Observational geometry | ||
| i | 38° | (a) |
| PA | 32° | (a) |
| d | 400 pc | (b) |
Notes. a(b) represents a × 10b. (1) The stellar spectrum is obtained by the sum of the accretion luminosity Lacc and an artificially high stellar luminosity L⋆ to shift the snowline to 47, 76, and 119 AU. (2) R⋆ is chosen to obtain an accretion luminosity of 4 × 102 L⊙, consistent with Cieza et al. (2016).
References.(a) Cieza et al. (2016), (b) Kounkel et al. (2017).
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