White dwarf eccentricity fluctuation and dissipation by AGB convection

Millisecond pulsars with white dwarf companions have typical eccentricities e~ 10⁻⁶-10⁻³. The eccentricities of helium white dwarfs are explained well by applying the fluctuation-dissipation theorem to convective eddies in their red giant progenitors. We extend this theory to more massive carbon-oxygen (CO) white dwarfs with asymptotic giant branch (AGB) progenitors. Due to the radiation pressure in AGB stars, the dominant factor in determining the remnant white dwarf's eccentricity is the critical residual hydrogen envelope mass mₑₙᵥ required to inflate the star to giant proportions. Using a suite of MESA stellar evolution simulations with Δ mc=10⁻³\, M_ core-mass intervals, we resolved the AGB thermal pulses and found that the critical mₑₙᵥ∝ mc⁻⁶. This steep dependence causes the e(mc) relation to turn over, such that e~ 3× 10⁻³ almost independently of the remnant CO white dwarf's mass mc. Nearly all of the measured eccentricities lie below this robust theoretical limit, indicating that the eccentricity is damped during the common-envelope inspiral that follows the unstable Roche-lobe overflow of the AGB star. Specifically, we focused on white dwarfs with median masses mc>0.6\, M_. These massive white dwarfs begin their inspiral with practically identical orbital periods and eccentricities, eliminating any dependence on the initial conditions. For this sub-sample, we find an empirical relation e∝ P3/2 between the final period and eccentricity that is much tighter than previous studies - motivating theoretical work on the eccentricity evolution during the common envelope phase.