– 9 – 2 4 6 8 0 1 2 3 Fig. 2.— Common envelope evolution for KOI-74. Lower (black) curve shows a$_{i}$ versus M 1 (0) for efficient envelope ejection. If the mass of the hot core detected by R2010 is in the brown-dwarf range, then the orbit may have been eccentric, and the massive donor star may have experienced a dynamical-time-scale instability at periastron. The high eccentricity would likely have been induced by interactions with a third star. Plotted in green are the possible orbital separations of the third star from the star monitored today by Kepler. Fig. 3.— M$_{c}$ versus log of the current orbital separation. Binaries that have experienced stable mass transfer (top panel); common envelope evolution (bottom panel). -2 -1 0 1 0.2 0.4 0.6 0.8 1 1.2 Log[(Semimajor Axis)/AU] 0.2 0.4 0.6 0.8 1 1.2