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

The structure and fate of white dwarf merger remnants