  The optical spectra of novae are characterized by emission lines from the
hydrogen Balmer series and either Fe II or He/N, leading to their traditional
classification into two spectral classes: "Fe II" and "He/N". For decades, the
origins of these spectral features were discussed in the literature in the
contexts of different bodies of gas or changes in the opacity of the ejecta,
particularly associated with studies by R. E. Williams and S. N. Shore. Here,
we revisit these major studies with dedicated, modern data sets, covering the
evolution of several novae from early rise to peak all the way to the nebular
phase. Our data confirm previous suggestions in the literature that the "Fe II"
and "He/N" spectral classes are phases in the spectroscopic evolution of novae
driven primarily by changes in the opacity, ionization, and density of the
ejecta, and most if not all novae go through at least three spectroscopic
phases as their eruptions evolve: an early He/N (phase 1; observed during the
early rise to visible peak and characterized by P Cygni lines of He I, N II,
and N III), then an Fe II (phase 2; observed near visible peak and
characterized by P Cygni lines of Fe II and O I), and then a later He/N (phase
3; observed during the decline and characterized by emission lines of He I. He
II, N II, and N III), before entering the nebular phase. This spectral
evolution seems to be ubiquitous across novae, regardless of their speed class;
however the duration of each of these phase differs based on the speed class of
the nova.
