Scenarios to explain extreme Be depletion in solar-like stars: accretion or rotation effects?

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Table 1

Parameters of strongly Be-depleted objects.

Star	T _eff	A(Be)	A(Li)	Age	vsini
	(K)			(Gyr)	(km s^-1)

HD 4391^a	5878	0.64	<1.09	1.2	2.72
HD 20766^a	5733	<−0.09	<0.97	1.6	1.98
HD 20807^a	5843	0.36	<1.07	2.1	1.74
HIP 17336^b	5671	<−0.85	<0.8	3.89	2.07
HIP 32673^b	5724	<−0.78	<1.0	3.16	2.83
HIP 64150^b	5800	<−0.88	<1.0	4.2	2.21
HIP 75676 ^b	5772	<−0.96	<1.1	4.16	2.18

Notes.

^(a)

From Santos et al. (2004);

^(b)

from Takeda et al. (2010) and Takeda et al. (2011).

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