  We present a numerical study of the mass transfer dynamics prior to the
gravitational wave-driven merger of a double white dwarf system. Recently,
there has been some discussion about the dynamics of these last stages,
different methods seemed to provide qualitatively different results. While
earlier SPH simulations indicated a very quick disruption of the binary on
roughly the orbital time scale, more recent grid-based calculations find
long-lived mass transfer for many orbital periods. Here we demonstrate how
sensitive the dynamics of this last stage is to the exact initial conditions.
We show that, after a careful preparation of the initial conditions, the
reportedly short-lived systems undergo mass transfer for many dozens of orbits.
The reported numbers of orbits are resolution-biased and therefore represent
only lower limits to what is realized in nature. Nevertheless, the study shows
convincingly the convergence of different methods to very similar results.
