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An intensive spectroscopic study was performed for three representative solartwins (HIP 56948, HIP 79672, and HIP 100963) as well as for the Sun (Moon;reference standard), with an intention of (1) quantitatively discussing therelative-to-Sun similarities based on the precisely established differentialparameters and (2) investigating the reason causing the Li abundancedifferences despite their similarities. It was concluded that HIP 56948 mostresembles the Sun in every respect including the Li abundance (though notperfectly similar) among the three and deserves the name of "closest-ever solartwin", while HIP 79672 and HIP 100963 have somewhat higher effectivetemperature and appreciably higher surface Li composition. While there is anindication of 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 produce themarked change in Li. Rather, this may be more likely to be attributed (at leastpartly) to the slight difference in T_eff via some T_eff-sensitiveLi-controlling mechanism. Since the abundance of beryllium was found to beessentially solar for all stars irrespective of Li, any physical processcausing the Li diversity should work only on Li without affecting Be.

High-Dispersion Spectroscopic Study of Solar Twins: HIP 56948, HIP 79672, and HIP 100963