  Of all the light elements, the evolution of lithium (Li) in the Milky Way is
perhaps the most difficult to explain. Li is difficult to synthesize and is
easily destroyed, making most stellar sites unsuitable for producing Li in
sufficient quantities to account for the proto-solar abundance. For decades,
novae have been proposed as a potential explanation to this 'Galactic Li
problem', and the recent detection of 7Be in the ejecta of multiple nova
eruptions has breathed new life into this theory. In this work, we assess the
viability of novae as dominant producers of Li in the Milky Way. We present the
most comprehensive treatment of novae in a galactic chemical evolution code to
date, testing theoretical- and observationally-derived nova Li yields by
integrating metallicity-dependent nova ejecta profiles computed using the
binary population synthesis code binary c with the galactic chemical evolution
code OMEGA+. We find that our galactic chemical evolution models which use
observationally-derived Li yields account for the proto-solar Li abundance very
well, while models relying on theoretical nova yields cannot reproduce the
proto-solar observation. A brief exploration of physical uncertainties
including single-stellar yields, the metallicity resolution of our nova
treatment, common-envelope physics, and nova accretion efficiencies indicates
that this result is robust to physical assumptions. Scatter within the
observationally-derived Li yields in novae is identified as the primary source
of uncertainty, motivating further observations of 7Be in nova ejecta.
