Table 6
Disk models for the Coronet cluster members.
Object | Teff (K) | R∗ (R⊙) | M∗ (M⊙) | Mdisk (M⊙) | amin − amax (μm) | Hrdisk/Rdisk | T(Rin) (K) | Rout (AU) | Comments | |
|
||||||||||
S CrA | 4500 | 3.60 | 1.5 | 3.8 × 10-2 | 0.1 − 10000 | 0.30 | 1500 | 400 | Massive, typical CTTS disk | |
T CrA | 7000 | 1.14 | 4.0 | 3.8 × 10-3 | 0.1 − 100 | 0.33 | 1500 | 300 | Typical CTTS disk | |
CrA-466 | 3500 | 1.06 | 0.4 | 2.8 × 10-4 | 0.1 − 100 | 0.1 | 1500 | 100 | Typical CTTS disk | |
CrA-45 | 3700 | 1.62 | 0.6 | 1.5 × 10-4 | 0.1 − 100 | 0.32 | 1500 | 100 | Typical CTTS disk | |
CrA-159 | 3500 | 1.95 | 0.4 | 3.8 × 10-6 | 0.1 − 100 | 0.33 | 1500 | 40 | Thick, truncated or strongly depleted. Gap? (continuous line) | |
′′ | 3500 | 1.95 | 0.4 | 5.4 × 10-6 | 0.1 − 20 | 0.33 | 1500 | 100 | Small grains only. Depleted. Gap? (dashed line) | |
HBC 677 | 3500 | 1.95 | 0.4 | 5.8 × 10-6 | 0.1 − 100 | 0.32 | 1500 | 100 | Low-mass disk, relatively thick | |
G-1 | 3900 | 2.50 | 0.6 | < 1.2 × 10-6 | 0.1 − 100 | 0.095 | 1500 | 100 | Very dust depleted and settled (dotted line) | |
′′ | 3900 | 2.50 | 0.6 | < 3 × 10-7 | 0.1 − 100 | 0.085 | 1500 | 30 | Settled, truncated (dashed line) | |
′′ | 3900 | 2.50 | 0.6 | < 6 × 10-7 | 0.1 − 20 | 0.095 | 1500 | 100 | Small grains only, depleted (continuous line) | |
G-14 | 3500 | 0.41 | 0.3 | < 9 × 10-7 | 0.1 − 100 | 0.08 | 1500 | 100 | Grain size differences between inner/outer disk | |
G-85a | 3800 | 1.60 | 0.6 | 1.7 × 10-4 | 0.1 − 2/0.1 − 100a | 0.09/0.095a | 1500/200a | 100 | Opt. thin inner disk/gap (pre-transitional)a | |
G-87 | 3700 | 1.15 | 0.5 | < 1.6 × 10-4 | 0.1 − 100 | 0.03 | 1500 | 100 | Standard disk model (dashed line) | |
′′ | 3700 | 1.15 | 0.5 | < 1.6 × 10-4 | 20 − 1000 | 0.02 | 1500 | 100 | Large grains (dotted line) | |
′′ | 3700 | 1.15 | 0.5 | < 1.6 × 10-4 | 20 − 1000 | 0.02 | 400 | 100 | Best fit: Inner hole plus large grains (continuous line) |
Notes. RADMC disk models for the Coronet cluster members. The stellar parameters (Teff, R∗) are determined from the optical observations and spectroscopy. The disk parameters are modified to reproduce the observed SED in the whole wavelength range, starting with the simplest possible model (see text). The disk masses are estimated assuming a gas-to-dust ratio of 100 and a collisional distribution for the dust with grain sizes amin − amax. In case of upper limits at PACS wavelengths, the corresponding disk masses are upper limits only.
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