Chemical Signatures of AGB Mass Transfer in Gaia White Dwarf Companions

Abstract We present a homogeneous abundance analysis of 160 main-sequence stars in astrometric white-dwarf + main-sequence (WD+MS) binaries with orbits from Gaia DR3. These systems have Astronomical unit-scale separations and are thought to have undergone mass transfer (MT) when the WD progenitor was an asymptotic giant branch (AGB) star. Using high-resolution spectroscopy, we measure chemical abundances of the MS stars, focusing on s -process elements. Since s -process nucleosynthesis occurs mainly in AGB stars, s -process enhancement in the MS star is a key signature of accretion from an AGB companion. We identify 43 barium dwarfs—39 of them newly discovered—roughly doubling the known population in astrometric WD+MS binaries and extending it to lower metallicities than previously studied. The s -process abundances show large star-to-star variations that correlate with component masses and with metallicity but not with orbital separation. At the lowest metallicities, three barium dwarfs display strong CH and C 2 absorption bands, confirming a link between barium stars and carbon enhanced metal-poor-s stars and implying that AGB mass transfer usually leads to strong carbon enhancement at low metallicity. By comparing the observed abundance patterns to AGB nucleosynthesis models, we show that the diversity of s -process enhancements can be explained by variations in donor mass, metallicity, and most importantly, the number of thermal pulses the AGB star experienced before the onset of MT. Variation in the depth of the accretors’ convective envelopes, with which accreted material is diluted, strengthens correlations with MS star mass and metallicity. Our results establish Gaia WD+MS binaries—which are homogeneously selected and probe shorter orbital periods than previous barium-star samples—as a powerful laboratory for constraining mass transfer physics and the origin of chemically peculiar stars.