  We present stellar evolution calculations of the remnant of the merger of two
carbon-oxygen white dwarfs (CO WDs). We focus on cases that have a total mass
in excess of the Chandrasekhar mass. After the merger, the remnant manifests as
an $L \sim 3 \times 10^4 L_\odot$ source for $\sim 10^4$ yr. A dusty wind may
develop, leading these sources to be self-obscured and to appear similar to
extreme AGB stars. Roughly $\sim 10$ such objects should exist in the Milky Way
and M31 at any time. As found in previous work, off-center carbon fusion is
ignited within the merger remnant and propagates inward via a carbon flame,
converting the WD to an oxygen-neon (ONe) composition. By following the
evolution for longer than previous calculations, we demonstrate that after
carbon-burning reaches the center, neutrino-cooled Kelvin-Helmholtz contraction
leads to off-center neon ignition in remnants with masses $\ge 1.35 M_\odot$.
The resulting neon-oxygen flame converts the core to a silicon WD. Thus,
super-Chandrasekhar WD merger remnants do not undergo electron-capture induced
collapse as traditionally assumed. Instead, if the remnant mass remains above
the Chandrasekhar mass, we expect that it will form a low-mass iron core and
collapse to form a neutron star. Remnants that lose sufficient mass will end up
as massive, isolated ONe or Si WDs.
