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Silicon abundances were determined by applying the spectrum-fitting technicto the Si II doublet lines at 6347 and 6371A for a sample of 120 main-sequencestars in the T_eff range of ~7000-14000K (comprising not only normal stars butalso non-magnetic chemically peculiar stars) with an aim of investigating theirbehaviors (e.g., correlation with stellar parameters and abundances of otherelements such as Fe or C) and the background physical mechanisms involvedtherein, where attention was paid to taking into account of the non-LTE effectand to assigning a reasonable value of microturbulence. The following trendswere revealed from the analysis: (i) The resulting [Si/H] values, mostlyranging from ~-0.5 to ~+0.3, show a positive correlation with [Fe/H]. (ii) Akind of anti-correlation exists between Si and C as seen from the tendency of[C/Si] steeply decreasing with [Si/H]. (iii) Si abundances do not show anyclear dependence upon T_eff or vsini, while Am and HgMn stars appear to showcomparatively higher [Si/H] than normal stars. Although it is notstraightforward to explain these observational facts, different physicalprocesses (gas-dust separation and atomic diffusion) are likely to beintricately involved in producing these characteristic behaviors of Sicomposition in the surface of late A through late B dwarfs.

Photospheric silicon abundances of upper main-sequence stars derived from Si II 6347/6371 doublet lines