Tracing the potential planet-forming regions around seven pre-main-sequence stars

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Volume 502 / No 1 (July IV 2009)

A&A, 502 1 (2009) 367-383

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Table 3:

Parameters of the models that simulate the measured SED and MIR visibilities best.
Object (model-no.)	$M_{\rm disk}$ [ $M_{\rm\odot}$ ]	$R_{\rm out}$ [AU]	$R_{\rm in}$ [AU]	$\beta$	$h_{\rm 100}$ [AU]	$\vartheta$ [ $^{\circ}$ ]	$\dot{M}$ [ $M_{\rm\odot}$ /a]
DR Tau (I)			0.10				$2.0 \times10^{-8}_{\rm (det.)}$
DR Tau (II)	0.1	90	0.10	0.75	15	20	$8.0 \times 10^{-8}_{\rm (1)}$
DR Tau (III)			0.05				$8.0 \times 10^{-8}_{\rm (det.)}$
GW Ori (I,II)	1.0	360	0.35	1.10	22	10	$2.5 \times 10^{-7}_{\rm (2)}$
HD 72106 B	0.005	40	0.50	1.30	8	60	No Accretion
RU Lup	0.1	100	0.10	0.90	20	28	$1.0 \times 10^{-8}_{\rm (3)}$
HBC 639	0.1	120	0.10	1.00	10	65	No Accretion
S CrA N (I)	0.03	120	0.05	1.10	9	10	$4.0 \times 10^{-8}_{\rm (det.)}$
S CrA N (II)				0.90	12	45
S CrA S	0.03	100	0.10	1.05	8	30	$4.0 \times 10^{-8}_{\rm (det.)}$

References: ⁽¹⁾: Akeson et al. (2005); ⁽²⁾: Calvet et al. (2002); ⁽³⁾: Herczeg et al. (2005).

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