  We propose a new method for determination of element abundances in stellar
atmospheres aimed for the automatic processing of high-quality stellar spectra.
The pan-spectral method is based on weighted cumulative line-widths Q of
studied element. Difference in quantities Q found from synthetic and observed
spectra gives a correction to the initial abundance. Final abundances are then
found by rapidly converging iterations. Calculations can be made for many
elements simultaneously and do not demand supercomputers.
