By ``MK Process,'' we label a specific methodology that makes possible the construction and use of systems of classification based on the particular observed characteristics of stellar spectra that have been selected to define the frames of reference. These systems must be autonomous; that is, they are to be defined completely by the appearance of the spectral features in arrays of standard stellar spectra, in a specified interval of wavelength.
Each of these autonomous systems must also be self-consistent; that
is, the array of individual standard stars must constitute - and
define - an orderly assemblage, from the point of view of the behavior
of the spectral lines, bands and patterns, within the spectral
intervals of the standard array. The interval 
3850-5000 has been
used most commonly in the past.
The autonomy of each array is achieved through its liberation from dependence on the results of stellar-atmospheric computations - or on any other theoretical models.
For such systems to be completely autonomous, we cannot require them to be attachable to the MK System - or to each other. They complement each other; but they each must live separate, independent lives.
Each new system is to be defined by a network of boxes (as in the MK System); and each of the boxes is to be defined by a specific stellar spectrum in a specific wavelength interval.
The increasing use of patterns, in place of the line ratios used principally earlier, can increase the discrimination in classification from both stellar spectrograms and stellar scans.