Abstract White dwarfs (WDs) receive natal velocity boosts of ∼1 km s −1 due to recoil from asymmetric mass loss during the late asymptotic giant branch (AGB) stage. In a wide binary, the acceleration of a WD progenitor exerts a torque, modifying the orbital eccentricity. Potential signatures of this effect have been detected in Gaia’s wide binary sample. At the same time, an AGB star’s puffy envelope facilitates strong tidal interactions in binaries with periapsis separations of a few astronomical units, capturing the companion into a tighter orbit and potentially driving the system towards a common-envelope phase. Using an analytical model for wide binary evolution under asymmetric AGB mass loss, we predict the eccentricity distribution of wide WD+MS and WD+WD binaries. We find that recoil can induce tidal interactions in up to ∼40% of initially wide binaries on the AGB or post-AGB for initial separations of ∼100–1000 au. We relate these interactions to three recent observational puzzles: (i) the dearth of wide WD+MS and WD+WD binaries in Gaia DR3 with eccentricities ≳0.9; (ii) the formation of moderately eccentric WD+MS and WD+WD binaries with orbital periods of ∼100–1000 days, which we suggest happens via a high-eccentricity common-envelope phase induced by recoil; and (iii) the origin of low-luminosity, long-timescale, dust-obscured transients towards AGB progenitors, such as the ongoing event WNTR23bzdiq in M31. Our findings have potential implications for the survival and dynamical evolution of planetary systems around WD progenitors, to be investigated in future works.
Christopher E. O’Connor (Tue,) studied this question.