Spectroscopic observations of novae date back a century and the
fundamental nature of the outburst has been understood for 50 years.
Yet, recent observations suggest a possible significant modification
to the standard nova paradigm.  A high-resolution spectroscopic survey
of novae has revealed short-lived heavy element absorption systems
near maximum light consisting of Fe-peak and s- process elements.  The
spectroscopic evolution of novae gives evidence for two distinct
interacting gas systems in which the bright continuum is produced by
the outburst ejecta but absorption and emission lines originate in gas
ejected by the secondary star in a way that could explain dust
formation and X-ray emission from novae. The absorbing gas is
circumbinary and it pre-exists the outburst.  Its origin appears to be
mass ejection from the accretion disk or secondary star, and it might
initiate the nova outburst.