Table 3
The peakiness parameter P10, the accretion luminosity and the line/continuum (L/C) ratio for a selected sample of protoplanetary disks.
| Index number | Source | P10a | L/C | Acc. lum. | Ref.b |
| [log(L⊙)] | |||||
|
|
|||||
| 1 | AA Tau | 1.8 (0.2) | 1.5 | –1.6 | 1 |
| 2 | AS 205 A | 11.5 (1.0) | 2.1 | 0.2c | 2 |
| 3 | CV Cha | 4.1 (0.8) | 1.3 | – | – |
| 4 | CW Tau | 3.0 (0.2) | 1.4 | –1.3 | 2 |
| 5 | DF Tau | 4.2 (0.5) | 1.5 | – 0.7 | 3 |
| 6 | DR Tau | 7.7 (0.8) | 2.9 | – 0.1 | 2 |
| 7 | DoAr24E A | 7.3 (2.0) | 1.5 | – 1.6 | 4 |
| 8 | DoAr 44 | 7.7 (0.3) | 1.4 | – | – |
| 9 | EX Lup | 10.8 (1.0) | 1.3 | – | – |
| 10 | FN Tau | 3.3 (0.5) | 1.5 | – | – |
| 11 | GQ Lup | 3.5 (0.5) | 1.4 | – | – |
| 12 | Haro 1-4 | 3.3 (0.5) | 1.4 | – | – |
| 13 | Haro 1-16 | 3.4 (0.4) | 1.3 | – | – |
| 14 | HD 135344B | 6.9 (0.3) | 1.2 | –0.9 | 5 |
| 15 | HD 142527 | 6.0 (0.5) | 1.2 | 0.0 | 5 |
| 16 | IRS 48 | 1.7 (0.2) | 1.2 | – | – |
| 17 | IRS 51 | 4.1 (0.4) | 1.2 | – | – |
| 18 | LkHa 330 | 5.2 (0.5) | 1.3 | – | – |
| 19 | RNO 90 | 4.5 (0.6) | 1.5 | – | – |
| 20 | RU Lup | 15.1 (3.5) | 1.8 | – 0.4 | 3 |
| 21 | RY Lup | 3.3 (0.5) | 1.2 | – | – |
| 22 | S CrA A | 13.4 (2.5) | 2.0 | – | – |
| 23 | S CrA B | 18.8 (2.3) | 1.8 | – | – |
| 24 | SR 9 | 2.4 (0.6) | 1.1 | –1.4 | 4 |
| 25 | SR 21 | 2.4 (0.3) | 1.2 | < –1.9 | 4 |
| 26 | TW Hya | 5.0 (0.5) | 2.3 | –1.4 | 3 |
| 27 | VSSG1 | 4.7 (1.0) | 1.5 | – 0.4 | 4 |
| 28 | VV CrA A | 14.0 (3.0) | 1.4 | – | – |
| 29 | VV Ser | 1.5 (0.2) | 1.1 | 1.2 | 5 |
| 30 | VW Cha | 8.1 (0.5) | 2.0 | – 0.2 | 6 |
| 31 | VZ Cha | 7.7 (0.6) | 2.2 | – 1.1 | 6 |
Values refer to an average of the lower J- transitions. Uncertainties are indicated in parentheses.
References. (1) Gullbring et al. (1998); (2) Valenti et al. (1993); (3) Herczeg & Hillenbrand (2008); (4) Natta et al. (2006); (5) Garcia Lopez et al. (2006); and (6) Hartmann et al. (1998).
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