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 diffusion/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 \pm 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 ; { T _ { eff } } \sim 7340 K , \log g \sim 4.1 , microturbulence \sim 4.3 { kms ^ { -1 } } , [ Fe/H ] \sim 0.50 .
This again provides distinct evidence for the effects of accretion in J37 and requires a new synthesis of the Be doublet .