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Lithium abundances and rotational behavior for bright giant stars
Aims.We study the links possibly existing between the lithium content ofbright giant stars and their rotational velocity. Methods: .Weperformed a spectral analysis of 145 bright giant stars (luminosityclass II) spanning the spectral range from F3 to K5. All these starshave homogeneous rotational velocity measurements available in theliterature. Results: .For all the stars of the sample, we provideconsistent lithium abundances (A_Li), effective temperatures (T_eff),projected rotational velocity (v sin i), mean metallicity ([Fe/H]),stellar mass, and an indication of the stellar multiplicity. The gradualdecrease in lithium abundance with T_eff is confirmed for bright giantstars, and it points to a dilution factor that is at least assignificant as in giant stars. From the F to K spectral types, the A_Lispans at least three orders of magnitude, reflecting the effects ofstellar mass and evolution on dilution. Conclusions: .We find thatthe behavior of A_Li as a function of v sin i in bright giant starspresents the same trend as is observed in giants and subgiants: starswith high A_Li are moderate or fast rotators, while stars with low A_Lishow a wide range of v sin i values.
| Variability of the emission-line spectra and optical continua of Seyfert galaxies. I
H-beta and O III forbidden line 4959,5007 A line strengths obtained fromnew observations of 27 broad line-emitting galaxies and six narrowline-emitting galaxies are compared with earlier measurements. It isfound that about 80% of broad line-emitting galaxies show significantchanges in their optical spectra, on time scales of less than about fiveyears. An analysis of changes in O II forbidden line/H-beta ratio for 24broad line-emitting galaxies shows that (1) changes in the H-beta fluxare correlated with changes in the optical continuum, providing evidencefor energy input into the line-emitting region by photoionization, and(2) in a number of galaxies, the structure of the broad emission linesin complex, with detailed line structure changes on time scales shorterthan about two months.
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