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High-Dispersion Spectroscopic Study of Solar Twins: HIP 56948, HIP 79672, and HIP 100963
An intensive spectroscopic study was performed for three representativesolar twins (HIP 56948, HIP 79672, and HIP 100963) as well as for theSun (Moon; reference standard), with intentions of (1) quantitativelydiscussing the relative-to-Sun similarities based on the preciselyestablished differential parameters and (2) investigating the reasonthat causes the Li abundance differences, despite their similarities. Itwas concluded that HIP 56948 most resembles the Sun in every respect,including the Li abundance (though not perfectly similar) among thethree, and deserves the name of ``closest-ever solar twin'', while HIP79672 and HIP 100963 have a somewhat higher effective temperature andappreciably higher surface Li composition. While there is an indicationof Li being rotation-dependent, because the projected rotation in HIP56948 (and the Sun) is slightly lower than the other two, the rotationaldifference alone does not seem to be so large as to efficiently producea marked change in Li. Rather, this may be more likely to be attributed(at least partly) to a slight difference in Teff via someTeff-sensitive Li-controlling mechanism. Since the abundanceof Be was found to be essentially solar for all stars irrespective ofLi, any physical process causing the Li diversity should work only on Liwithout affecting Be.
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