Table B.2
Reference sample of protoplanetary disc-hosting stars for comparison.
System | Age | C | O | Fe | log10(Ṁacc) | Meeus |
---|---|---|---|---|---|---|
HD 31648 | 6.2 | −3.63 ± 0.07 | −3.24 ± 0.05 | −4.43 ± 0.13 | −6.9 | IIa |
HD 163296 | 4.1 | −3.78 ± 0.25 | −3.27 ± 0.15 | −4.35 ± 0.15 | −7.16 | IIa |
HD 244604 | 1.9 | −3.65 ± 0.17 | −3.19 ± 0.08 | −4.31 ± 0.24 | −7.2 | IIa |
HD 190073 | 1.6 | −3.68 ± 0.14 | −3.22 ± 0.11 | −4.38 ± 0.06 | −8.68 | IIa |
HD 104237 | 2.06 | −3.58 ± 0.20 | −3.17 ± 0.15 | −4.39 ± 0.18 | −7.45 | IIa |
HD 142666 | 6.9 | −3.58 ± 0.15 | −3.14 ± 0.15 | −4.80 ± 0.11 | −7.77 | IIa |
HD 144432 | 5.5 | −3.75 ± 0.18 | −3.13 ± 0.10 | −4.66 ± 0.09 | −7.74 | IIa |
HD 101412 | 1.2 | −3.54 ± 0.12 | −3.08 ± 0.09 | −5.04 ± 0.19 | −7.04 | IIa/Ia |
HD 31293 | 2.6 | −3.29 ± 0.22 | −3.23 ± 0.20 | −4.87 ± 0.22 | −7.74 | Ia |
HD 36112 | 1.5 | −3.57 ± 0.16 | −3.14 ± 0.10 | −4.45 ± 0.14 | −6.05 | Ia |
HD 179218 | 1.1 | −3.41 ± 0.16 | −3.06 ± 0.13 | −4.99 ± 0.13 | −6.72 | Ia |
HD 100546 | 10 | −3.68 ± 0.20 | −3.25 ± 0.20 | −5.67 ± 0.08 | −7.23 | Ia |
HD 250550 | 0.25 | − | − | −5.36 ± 0.12 | −7.8 | Ia |
HD 142527 | 0.86 | − | − | −4.59 | −7.16 | Ia |
HD 139614 | 13.5 | −3.71 ± 0.22 | −3.29 ± 0.10 | −5.03 ± 0.13 | −7.99 | Ia |
HD 34282 | 7.81 | − | − | −5.3 ± 0.1 | −7.71 | Ib |
HD 141569 | 4 | −3.59 ± 0.29 | −3.01 ± 0.10 | −5.21 ± 0.32 | −8.37 | Ib |
HD 169142 | 8.5 | −3.51 ± 0.12 | −3.34 ± 0.13 | −5.09 ± 0.11 | −7.4 | Ib |
HD 100453 | 10 | −3.44 ± 0.09 | − | −4.57 ± 0.19 | −8.04 | Ib |
HD 135344B | 8.93 | − | − | −4.56 ± 0.10 | −7.69 | Ib |
HD 245185 | 5.5 | −3.68 ± 0.15 | −3.13 ± 0.17 | −5.23 ± 0.33 | −7.2 | I |
Notes. The stellar abundances are taken from Kama et al. (2015, and references therein). The Meeus column identifies the specific Meeus group (Meeus et al. 2001) to which the star belongs, with the "a" and "b" sub-classifications based on the presence or absence of emission features from warm, small silicate grains, respectively.
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