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Table 3

Predicted binary signatures from the models of Artymowicz & Lubow (1994), projection effects caused by the inclination of the orbit, and hole/gap range where stellar/substellar companions can be ruled out from the NACO images.

Star R hole,out Model 11 Model 22 Model 33 i Proj. effects4 ΔRstellar5 ΔRsubstellar6
d S P d S P d S P d proj ∗ d proj ∗∗
(AU) (AU) (yr) (AU) (yr) (AU) (yr) (deg) (AU) (AU) (AU) (AU)
DoAr 21 100 59 276 29−48 95−202 7.6−53 13−235  <45 42−59 71−100 12.2−100 31−100
HD 135344B 39 23 69 11−19 23−52 3−21 3−60 21 21−23 36−39 14−39 37−39
HR 4796A 69 41 136 20−33 46−98 5−37 6−116 76 10−41 17−69 7.3−69 13−69
T Cha 15 8.8 17.4 4.3−7.2 6−13 1.1−7.9 0.8−15 60 or 75 2.3−8.8 4−15 10.8−15 –
TW Hya 4.3 2.53 4.2 1.25−2.1 1.5−3.2 0.33−2.3 0.2−3.7 4.3 2.52−2.53 4.29−4.3 – –

Notes. 

(1)

Model 1 (circular orbit): e = 0, Rhole,out = 1.7a and the distance of the secondary relative to the primary is dS = a = Rhole,out/1.7.

(2)

Model 2: e = 0.25, Rhole,out = 2.6a and a(1 − e) < dS < a(1 + e) or 0.29   Rhole,out < dS < 0.48   Rhole,out.

(3)

Model 3: e = 0.75, Rhole,out = 3.3a and a(1 − e) < dS < a(1 + e) or 0.076   Rhole,out < dS < 0.53   Rhole,out.

(4)

Binary coplanar with the disk (iS = idisk), circular orbit (e = 0), xproj = a   cos   θ, yproj = a   sin   θ   cos   i and ; dproj(max) = a for θ = 0° and dproj(min) = a   cos   i for θ = 90°. Computed for  ∗ a = Rhole,out/1.7 and  ∗  ∗ a = Rhole,out.

(5)

Range of disk hole radii, starting at 01 from the primary, in which stellar binary companions can be ruled out on basis of the VLT/NACO images and using the BT-DUSTY evolutionary models.

(6)

Range of disk hole radii in which substellar binary companions can be ruled out from this work.

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