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We calculate the long-term evolution of angular momentum in double whitedwarf binaries undergoing direct impact accretion over a broad range ofparameter space. We allow the rotation rate of both components to vary, andaccount for the exchange of angular momentum between the spins of the whitedwarfs and the orbit, while conserving the total angular momentum. We includegravitational, tidal, and mass transfer effects in the orbital evolution, andallow the Roche radius of the donor star to vary with both the stellar mass andthe rotation rate. We examine the long-term stability of these systems,focusing in particular on those systems that may be progenitors of AM CVn orType Ia Supernovae. We find that our analysis yields an increase in thepredicted number of stable systems compared to that in previous studies.Additionally, we find that by properly accounting for the effects ofasynchronism between the donor and the orbit on the Roche-lobe size, weeliminate oscillations in the orbital parameters which are found in previousstudies. Removing these oscillations can reduce the peak mass transfer rate insome systems, keeping them from entering an unstable mass transfer phase.

Long-term evolution of double white dwarf binaries accreting through direct impact