No longer impossible: the self-lensing binary KIC 8145411 is a triple

Abstract

Five self-lensing binaries (SLBs) have been discovered with data from the \textit{Kepler} mission. One of these systems is KIC 8145411, which was reported to host an extremely low mass (ELM; $0.2M_{\odot }$) white dwarf (WD) in a 456-day orbit with a solar-type companion. The system has been dubbed "impossible", because evolutionary models predict that $\sim 0.2M_{\odot }$ WDs should only be found in tight orbits ($P_{\mathrm{orb}}\lesssim$ days). In this work, we show that KIC 8145411 is in fact a hierarchical triple system: it contains a WD orbiting a solar-type star, with another solar-type star $\sim 700$AU away. The wide companion was unresolved in the Kepler light curves, was just barely resolved in Gaia DR3, and is resolved beyond any doubt by high-resolution imaging. We show that the presence of this tertiary confounded previous mass measurements of the WD for two reason: it dilutes the amplitude of the self-lensing pulses, and it reduces the apparent radial velocity (RV) variability amplitude of the WD's companion due to line blending. By jointly fitting the system's light curves, RVs, and multi-band photometry using a model with two luminous stars, we obtain a revised WD mass of $(0.53\pm 0.01)M_{\odot }$. Both luminous stars are near the end of their main-sequence evolution. The WD is thus not an ELM WD, and the system does not suffer the previously proposed challenges to its formation history. Similar to the other SLBs and the population of astrometric WD binaries recently identified from Gaia data, KIC 8145411 has parameters in tension with standard expectations for formation through both stable and unstable mass transfer. The system's properties are likely best understood as a result of unstable mass transfer from an AGB star donor.

16 pages, 13 figures, Published in PASP

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• White dwarf eccentricity fluctuation and dissipation by AGB convection
• Two unseen massive white dwarf candidates in close binaries
• Direct detections of white dwarfs in four WD+dM post-common envelope binaries within 20 pc