Table 1
Properties of the stars of the T Tauri sample.
| # | Name | Sp. type | Teff | L | d | M | Age | Ṁacc | References |
|---|---|---|---|---|---|---|---|---|---|
| (K) | (L⊙) | (pc) | (M⊙) | (Ma) | (M⊙ yr−1) | ||||
| 1 | DG Tau | K6 | 4200 | 1.58 ± 0.37 | 125.2 ± 2.3 | 0.8 ± 0.2 | 1–2 | 4.6–74 10−8 | White & Ghez (2001) |
| 2 | DR Tau | K5 | 4450 | 3.48 ± 0.61 | 193.0 ± 1.9 | 1.0 ± 0.2 | ≤1 | 5.2 10−8 | Ingleby et al. (2013) |
| 3 | RY Tau | K1 | 5170 | 11.5 ± 3.8 | 138.2 ± 4.8 | 2.7 ± 0.3 | 1–2 | 6–9 × 10−9 | Calvet et al. (2004) |
| 4 | T Tau N | K0 | 5280 | 10.4 ± 2.7 | 145.1 ± 1.0 | 2.6 ± 0.3 | 1–2 | 3–5 × 10−8 | Calvet et al. (2004) |
| 5 | GQ Lup | K7 | 4050 | 1.52 ± 0.68(a) | 154.1 ± 0.9 | 0.6 ± 0.2 | 1–2 | 2 × 10−8 | Alcala et al. (2017) |
| 6 | IM Lup | M0 | 3850 | 2.51 ± 1.15(a) | 155.8 ± 1.0 | 0.4 ± 0.2 | ≤1 | 6.3 × 10−9 | Alcala et al. (2017) |
| 7 | RU Lup | K7 | 4050 | 1.64 ± 0.22 | 157.5 ± 1.3 | 0.6 ± 0.2 | 1–2 | 4–11 × 10−8 | Alcala et al. (2017) |
| 8 | RY Lup | K2 | 5040 | 2.36 ± 0.41(b) | 153.5 ± 1.8 | 1.7 ± 0.2 | 3–6 | 6.3 × 10−9 | Alcala et al. (2017) |
| 9 | S CrA N | K5–6 | 4300 | 3.82 ± 0.54 | 160.5 ± 2.2 | 0.9 ± 0.2 | ≤1 | 10−7 | Sullivan et al. (2019) |
| 10 | S CrA S | K5–6 | 4300 | 1.44 ± 0.07 | 147.4 ± 2.1 | 0.9 ± 0.2 | 1–2 | 3 × 10−8 | Sullivan et al. (2019) |
| 11 | VV CrA SW(*) | K7 | 4050 | 1.73 ± 0.24 | 156.6 ± 1.2 | 0.6 ± 0.2 | 1–2 | 2–3 × 10−8 | Sullivan et al. (2019) |
| 12 | V2062 Oph | K2–3 | 4840 | 1.61 ± 0.21(c) | 146.3 ± 0.6 | 1.5 ± 0.2 | 3–6 | 6.3 × 10−9 | Manara et al. (2014) |
| 13 | V2129 Oph | K5 | 4450 | 2.51 ± 0.54 | 131.9 ± 0.5 | 1.0 ± 0.2 | 1–2 | 1.5 × 10−9 | Alencar et al. (2012) |
| 14 | AS 205 N | K0 | 5280 | 3.89 ± 0.98 | 132.1 ± 1.6 | 1.9 ± 0.2 | 2–6 | 7.2 × 10−7 | Eisner et al. (2005) |
| 15 | AS 353 | K5 | 4450 | 3.90 ± 0.67(d) | 399.6 ± 4.2 | 1.0 ± 0.2 | ≤1 | 7.9 × 10−8 | Rei et al. (2018) |
| 16 | DI Cha | G2 | 5770 | 15.1 ± 4.8 | 189.0 ± 0.6 | 2.4 ± 0.4 | 2–5 | 5.98 × 10−8 | Antoniucci et al. (2011) |
| 17 | TW Hya | K6 | 4200 | 0.41 ± 0.05 | 60.14 ± 0.07 | 0.9 ± 0.1 | 4–12 | 2 × 10−9 | Manara et al. (2014) |
Notes. The effective temperatures are derived from the spectral types. Unless noted otherwise, the intrinsic luminosities are taken from Varga et al. (2018) and rescaled with distances from Gaia EDR3 (Gaia Collaboration 2021). The masses and the ages are derived from the evolutionary PISA tracks (Tognelli et al. 2011) displayed in Fig. 1. The accretion rates are taken from the references given in the last column of the Table. (a) L from Alcala et al. (2017). (b) L from Gravity Collaboration (2020a) with an error of 15%. (c)L from Bouvier et al. (2020a). (d)L from Hamann & Persson (1992) with an error of 15%. (*)This component is also called VV CrA South or VV CrA A.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.