Protostars, multiplicity, and disk evolution in the Corona Australis region: a Herschel Gould Belt Study

A. Sicilia-Aguilar; T. Henning; H. Linz; P. André; A. Stutz; C. Eiroa; G. J. White

doi:10.1051/0004-6361/201220170

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Volume 551 (March 2013)

A&A, 551 (2013) A34

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Table 6

Disk models for the Coronet cluster members.

Object	T_eff (K)	R_∗ (R_⊙)	M_∗ (M_⊙)	M_disk (M_⊙)	a_min − a_max (μm)	H_rdisk/R_disk	T(R_in) (K)	R_out (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-85^a	3800	1.60	0.6	1.7 × 10^-4	0.1 − 2/0.1 − 100^a	0.09/0.095^a	1500/200^a	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 (T_eff, 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 a_min − a_max. 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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