Abstract
There is given a summary of observational and theoretical aspects dealt with in the solar abundance determination. The solar abundance of sixty-six chemical elements are known. The abundance of some of these elements are based on one spectral line only (Ga, Ge, Sn, Er, Yb, Lu, Au, and Th) and the results may be erroneous. For six elements (B, Cs, Hg, Tl, Bi, and U) are given only upper limits for the abundance. Lines of Ho and Tb are suspected in the solar spectrum, but so far the abundances of these elements are not determined.
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