The CHIANTI database is quite flexible and can be easily adapted for use in a number of situations. Its uses include the calculation of temperature- and density-sensitive line ratios such as shown in Figs. 3 (click here) and 4 (click here). The numerator in the Si IX line ratio in Fig. 4 (click here) sums the contributions of two lines that would be blended by spectrographs with resolving powers that are currently available. Blending is a common problem and can be readily assessed with the CHIANTI database.
Another intended use of the CHIANTI database is for computations of synthetic spectra for comparison with observed spectra, regardless of spectral resolution. Again, blending can be an important aspect of these studies. A synthetic spectrum of a quiet solar region at wavelengths between 160 and 200 Å is shown in Fig. 5 (click here), for a FWHM spectral resolution of 0.2 Å.