UVES Be observations of early-G dwarfs in old clusters

Details UVES Be observations of early-G dwarfs in old clusters UVES Be observations of early-G dwarfs in old clusters

2002-03-11

arxiv.org/abs/astro-ph/0203155v1

Astronomy and Astrophysics

Astrophysics

to appear in A&A

Scientific paper

10.1051/0004-6361:20020355

We have obtained the first beryllium measurements of late F/early G-type stars in the old open cluster M67 (4.5 Gyr) and in the intermediate age cluster IC 4651 (1.7 Gyr). One member of the young cluster IC 2391 (~50 Myr) was also observed. Our sample stars have effective temperatures within a range of +30 - +380 K from the solar temperature. All our sample stars, including the Sun and the young cluster star have, within the errors, the same Be abundance. This result implies that late F/early G-type stars undergo very little (if any) Be depletion during their main-sequence life-time. Since these stars have undergone some Li depletion, our finding is indicative of shallow mixing, i.e. of a mixing process that can transport surface material deep enough for Li burning to occur, but not deep enough for Be burning. As shown in previous studies, the Li vs. Be diagram is a powerful diagnostic of stellar interiors. In this context, we do not find any evidence of correlated Li and Be depletion; furthermore, a comparison with various models shows that the Be pattern of our sample stars is compatible only with models including gravity waves. This class of models, however, cannot reproduce the Li observations of M 67.

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