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The equivalent widths (W) of 565 spectral lines in the wavelength range of4690--6870A were evaluated at 31 consecutive points from the solar disk center(mu=cos(theta)=1) to near the limb (mu=0.25) by applying the syntheticspectrum-fitting technique, in order to clarify the nature of theircenter--limb variations, especially the observed slope differing from line toline and its interpretation in terms of line properties. We found that thedistribution of the gradient beta (= -dlog W/dlog mu) well correlates with thatof dlog W/dlog T index, which means that the center-to-limb variation of W isdetermined mainly by the T-sensitivity of individual lines because theline-forming region shifts towards upper layers of lower T as we go toward thelimb. Further, the key to understanding the behavior of dlog W/dlog T(depending on the temperature sensitivity of number population) is whether theconsidered species is in minor population stage or major population stage, bywhich the distribution of beta is explained in terms of differences inexcitation potential and line strengths. All the center--limb data ofequivalent widths (as well as line-of-sight turbulent velocity dispersions,elemental abundances, and mean line-formation depths derived as by-products)along with the solar spectra used for our analysis are made available ason-line materials.

Solar Center--Limb Variation of the Strengths of Spectral Lines: Classification and Interpretation of Observed Trends