Table 1.
Atmosphere parameters and Li abundances (derived using hydrostatic models) and other selected observational information.
| IRAS name | Teff (K) | log g | νexp(OH) (km s−1) | Ref. | Period (days) | Ref. | log ε(Li)static |
|---|---|---|---|---|---|---|---|
| 01085+3022 | 3300 | −0.5 | 13 | 1 | 560 | 1 | 2.4 |
| 02095−2355 | 3300 | −0.5 | 12† | … | 659 | 2 | 1.6 |
| 05027−2158 | 2800 | −0.5 | 8 | 2 | 368 | 1 | 1.1 |
| 05098−6422 | 3000 | −0.5 | 6 | 3 | 394 | 3 | ≤−1.0 |
| 05151+6312 | 3000 | −0.5 | 15 | 3 | 628 | 4 | <0.0 |
| 05559+3825 | 2900 | −0.5 | 12† | 6 | 590 | 5 | 0.6 |
| 06300+6058 | 3000 | −0.5 | 12 | 3 | 440 | 6 | 0.7 |
| 07304−2032 | 2700 | −0.5 | 7 | 4 | 509 | 1 | 0.9 |
| 09429−2148 | 3300 | −0.5 | 12 | 3 | 650 | 1 | 2.2 |
| 10261−5055 | 3000 | −0.5 | 4 | 2 | 317 | 1 | ≤−1.0 |
| 11081−4203 | 3000 | −0.5 | 8† | 2 | 332 | 8 | 1.3 |
| 14266−4211 | 2900 | −0.5 | 9 | 2 | 389 | 8 | ≤0.0 |
| 14337−6215 | 3300 | −0.5 | 20 | 5 | … | … | 2.41 |
| 15193+3132 | 2800 | −0.5 | 3 | 3 | 360 | 1 | ≤0.0 |
| 15211−4254 | 3300 | −0.5 | 11 | 2 | … | … | 2.3 |
| 15255+1944 | 2900 | −0.5 | 7 | 3 | 425 | 1 | 1.0 |
| 15576−1212 | 3000 | −0.5 | 10 | 3 | 415 | 1 | 1.1 |
| 16030−5156 | 3000 | −0.5 | 10† | 2 | 579 | 9 | 1.5 |
| 16037+4218 | 2900 | −0.5 | 4 | 2 | 360 | 10 | ≤−1.0 |
| 16260+3454 | 3300 | −0.5 | 12 | 3 | 475 | 1 | 2.7 |
| 17034−1024 | 3300 | −0.5 | 8† | 2 | 346 | 1 | ≤0.0 |
| 18413+1354 | 3300 | −0.5 | 15 | 6 | 590 | 5 | 1.8 |
| 18429−1721 | 3000 | −0.5 | 7 | 2 | 481 | 8 | 1.2 |
| 19129+2803 | 3300 | −0.5 | 11† | 2 | 420 | 10 | 3.11 |
| 19361−1658 | 3000 | −0.5 | 8 | 2 | … | … | 1.9 |
| 20052+0554 | 3300 | −0.5 | 16 | 7 | 450 | 5 | 2.6 |
| 20343−3020 | 3000 | −0.5 | 8 | 2 | 349 | 1 | ≤−1.0 |
| RU Cyg | 3000 | −0.5 | 12† | … | 442 | 11 | 2.0 |
| SV Cas | 3000 | −0.5 | 12† | … | 456 | 11 | 3.5 |
| R Cen | 3000 | −0.5 | 5† | … | 251 | 11 | 4.3 |
Notes. (†)These stars only display a single peak in the 1612 MHz OH maser. Thus, in the abundance analysis, we adopted the average OH expansion velocities from the velocity values displayed by the other sample stars with similar variability periods. (1)The line is resolved in two components (circumstellar and photospheric) and the abundance obtained corresponds to the photospheric one.
References. References for the OH expansion velocities: (1) Chengalur et al. (1993); (2) te Lintel Hekkert et al. (1991); (3) te Lintel Hekkert et al. (1989); (4) Sivagnanam et al. (1989); (5) Sevenster et al. (1997); (6) Slootmaker et al. (1985); (7) Lewis (1994). References for the periods: (1) Combined General Catalogue of Variable Stars (GCVS), Kholopov et al. (1998); (2) Richards et al. (2012); (3) Whitelock et al. (1994); (4) Woźniak et al. (2004); (5) Jones et al. (1990); (6) Lockwood (1985); (7) Groenewegen & de Jong (1998); (8) AAVSO International Variable Star Index, Watson et al. (2006); (9) General Catalogue of Variable Stars (GCVS), Samus’ et al. (2017); (10) Jiménez-Esteban et al. (2006), (11) García-Hernández et al. (2013).
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