Born-again Protoplanetary Disk around Mira B

TheMiraAB system is a nearby ( 107 pc) example of awind accreting binary star system. In this class of system, the wind from amass-losing red giant star (Mira A) is accreted onto a companion (Mira B), as indicated by an accretion shock signature in spectra at ultraviolet and X-ray wavelengths. Using novel imaging techniques, we report the detection of emission at mid-infrared wavelengths between 9.7 and 18.3 m from the vicinity of Mira B but with a peak at a radial position about 10AU closer to the primaryMiraA.We interpret themid-infrared emission as the edge of an optically-thick accretion disk heated by Mira A. The discovery of this new class of accretion disk fed by M-giant mass loss implies a potential population of young planetary systems in white dwarf binaries, which has been little explored despite being relatively common in the solar neighborhood. Subject headinggs: binaries: symbiotic — stars: AGB and post-AGB — stars: individual (Mira AB) — stars: winds, outflows — techniques: interferometric