  We present a large parameter study where we investigate the structure of
white dwarf (WD) merger remnants after the dynamical phase. A wide range of WD
masses and compositions are explored and we also probe the effect of different
initial conditions. We investigated the degree of mixing between the WDs, the
conditions for detonations as well as the amount of gas ejected. We find that
systems with lower mass ratios have more total angular momentum and as a result
more mass is flung out in a tidal tail. Nuclear burning can affect the amount
of mass ejected. Many WD binaries that contain a helium-rich WD achieve the
conditions to trigger a detonation. In contrast, for carbon-oxygen transferring
systems only the most massive mergers with a total mass above ~2.1 solar masses
detonate. Even systems with lower mass may detonate long after the merger if
the remnant remains above the Chandrasekhar mass and carbon is ignited at the
centre. Finally, our findings are discussed in the context of several possible
observed astrophysical events and stellar systems, such as hot subdwarfs, R
Coronae Borealis stars, single massive white dwarfs, supernovae of type Ia and
other transient events. A large database containing 225 white dwarf merger
remnants is made available via a dedicated web page.
