Table 1.
Stellar sample S1.
| HD | log ϵ(Li) | NLTE | Vrot sin i | IR excess |
Tdust | |
|---|---|---|---|---|---|---|
| (km s−1) | short | far | (K) | |||
| Li-rich K giants | ||||||
| 787 | 1.99 | Y | 1.5 | N | N | |
| 6665 | 2.93 | Y | 2.3 | N | – | |
| 9746 | 3.44 | Y | 5.5 | N | – | |
| 30834 | 1.98 | Y | 0. | N | Y (e) | |
| 39853 | 2.75 | Y | 1.2 | N | N | |
| 40827 | 2.05 | Y | 0. | N | – | |
| 63798 | 2.00 | Y | 1.2 | N | – | |
| 90633 | 2.18 | Y | 0. | N | – | |
| 112127 | 2.95 | Y | 0. | N | – | |
| 116292 | 1.65 | Y | 0. | N | – | |
| 233517 | 3.95 | Y | 19.7 | Y | Y | 70 (f) |
| Non-Li-rich K giants | ||||||
| 6 | 0.37 (c) | N | 0. | N | N | |
| 3627 | 0.20 (c) | N | 0. | N | Y (e) | |
| 21078 | 1.30 | N | 0. | N | – | |
| 27497 | <0.40 | N | 0. | N | – | |
| 31553 | 0.5 (b) | N | 0. | N | – | |
| 34043 | < − 0.43 | N | 0. | N | – | |
| 43827 | <0.00 | N | 0. | N | – | |
| 108471 | – | – | 0. | N | – | |
| 119853 | <0.4 (b) | N | 0. | N | Y (d) | 68 |
| 153687 | 0.10 | N | 1.2 | N | Y (d)(e) | 74 |
| 156115 | < − 1.0 (b) | N | 1.2 | N | Y (d) | 38 |
| 212320 | 0.87 (a) | Y | 0.8 | N | Y (d) | 46 |
| 221776 | < − 1 (b) | N | 1.0 | Y | Y (d) | 59 |
Notes. Stars with a confirmed IR excess appear in bold face. The column labelled Tdust lists the dust temperature derived by Kim et al. (2001) from their ISO data and based on a detached-shell model, except for HDE 233517 for which this information comes from the analysis by Jura (2003) under the assumption of a flared disk. The column labelled “NLTE” indicates whether NLTE corrections have been applied to the Li abundance, whereas column Vrot sin i lists a proxy for the rotational velocity (see text).
excess confirmed by ISO data (Kim et al. 2001);
excess confirmed by AKARI data (Murakami et al. 2007);
temperature at the outer edge of a flared disk (Jura 2003).
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