Table 1
Properties of WTTs observed by CoRoT and modelled in this investigation.
| CoRoT ID | Mon-ID | Sp. type | Sp. Ref. | R | R Ref. | Ic | Ic Ref. | EW Hα | Hα Ref. | τe | ϵ |
| (mag) | (mag) | (Å) | (s) | ||||||||
|
|
|||||||||||
| 223959652 | 1256 | G0 | 1 | 12.85 | 4 | 12.47 | 4 | –3.32 | 6 | 32 | 1.432 × 10-4 |
| 616849446 | 565 | K4.5 | 2 | 13.94 | 5 | 13.19 | 5 | 1.60 | 2 | 32 | 2.756 × 10-4 |
| 223982407 | 33 | K5 | 2 | 14.47 | 4 | 13.76 | 4 | 1.40 | 2 | 512 | 1.212 × 10-3 |
| 223988965 | 695 | K6 | 1 | 14.11 | 4 | 13.31 | 3 | 1.30 | 6 | 512 | 4.683 × 10-4 |
| 616919771 | 784 | K5 | 1 | 14.06 | 4 | 13.33 | 4 | 1.83 | 6 | 512 | 3.488 × 10-4 |
Reference. 1 Makidon et al. (2004); 2 Dahm & Simon (2005); 3 Sung et al. (2008), Table 3 (photometry obtained at the Canada-France-Hawaii Telescope); 4 Sung et al. (2008), Table 8 (SSO WFI photometry, after adding 0.067 to the I magnitude so to homogenize it with Table 3); 5 Lamm et al. (2004); and 6 Rebull et al. (2002).
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