In September 2002 the discovery of a super Li-rich F-dwarf (J37) in NGC 6633, an iron poor analogue of the better studied Hyades and Praecepe open clusters, was announced. This unique star was thought to be the smoking gun for the action of diﬀusion, models of which predict a narrow ”Li-peak” at approximately the correct temperature. However, with more detailed studies into J37s abundance pattern this star provides ﬁrm evidence for the accretion of planetesimals or other material from the circumstellar environment of new born stars. Thanks to the speciﬁc predictions made about the behaviour of Be abundances, (the most striking of which being no Be in super-Li-rich dwarfs subject to diﬀusion) the opposing diﬀu-sion/accretion predictions can be tested. Initial modelling of the Be line indicates that J37 is as Be rich as it is Li rich; log N(Be) = 2.25 ± 0.25, and so is broadly consistent with an accretion-fuelled enhancement. However, that both Li and Be are enhanced by much more than the iron-peak elements (as determined in previous studies) suggests that diﬀusion also plays a role in increasing the abundances of Li and Be speciﬁcally. Furthermore, a new data set from the UVES/UT2 combination has allowed the elemental abundance of Iron to be measured, and the set of preliminary stellar parameters determined; Teﬀ ∼ 7340 K, log g ∼ 4.1, microturbulence ∼ 4.3 kms− 1, [Fe/H] ∼ 0.50. This again provides distinct evidence for the eﬀects of accretion in J37 and requires a new synthesis of the Be doublet.
The Li Overabundance of J37: Diﬀusion or Accretion?Publications
PublisherThe A-Star Puzzle Proceedings IAU Symposium
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