  Nova 1670 is a historical transient bearing strong similarities to a
recently-recognized type of stellar eruptions known as red novae, which are
thought to be powered by stellar mergers. The remnant of the transient, CK Vul,
is observable today mainly through cool circumstellar gas and dust, and
recombining plasma, but we have no direct view on the stellar object. Within
the merger hypothesis, we aim to infer the most likely makeup of the progenitor
system that resulted in Nova 1670. We collect and summarize the literature data
on the physical properties of the outburst and the remnant, and on the chemical
composition of the circumstellar material which resulted from optical and
submillimeter observations of the circumstellar gas of CK Vul. Simple
simulations yield the form and level of mixing of material associated with the
merger. Products of nuclear burning are identified, among them ashes of H
burning in the CNO cycles and the MgAl chain, as well as of partial He burning.
Based on the luminosity and chemical composition of the remnant, we find that
the progenitor primary had to be an evolutionarily advanced red-giant branch
star of a mass of 1-2 M$_{\odot}$. The secondary was either a very similar
giant, or a He white dwarf. While the eruption event was mainly powered by
accretion, we estimate that about 12% of total energy might have come from He
burning activated during the merger. The coalescence of a first-ascent giant
with a He white dwarf created a star with a rather unique internal structure
and composition, which resemble these of early R-type carbon stars. Nova 1670
was the result of a merger between a He white dwarf and a first-ascent red
giant and is likely now evolving to become an early R-type carbon star.
