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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.

(a)

Marks objects with a distinct inner and outer disks, so the given values correspond to the inner and outer disk. In case of different models, the comments include a reference to the appropriate figure.

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