white dwarfs will be mistaken for transiting planets. The two red circles shown in this panel correspond to KOI-74 (on the left) and KOI-81 (on the right and slightly higher). Although lensing has not been considered in the light- curve modeling of KOI-74 and KOI-81 carried out by R2010 and vK2010, there was no indication that it was needed. And clearly lensing did not cancel the effect of the transits, since Kepler did detect these events. The position of KOI-74 on the graph of M$_{WD}$ versus log ( a/ AU) indicates that R$_{E}$/R$_{WD}$ is expected to be small, so that lensing should not be significant. In fact, the radius of KOI-74b is larger than typical of a white dwarf of this mass (R2010), indicating that it may still be cooling. We find R$_{E}$/R$_{WD}$ is approximately 0 . 1 . The position of KOI-81 on the graph of M$_{WD}$ versus log ( a/ AU) indicates that, if the radius of KOI-81b satisfies the mass/radius relationship for white dwarfs, lensing effects may be important. R2010 find, however, that the radius of KOI-81b is 0 . 115 R ⊙ , placing it near the top of the cooling curve. The value of R$_{E}$/R$_{WD}$ is ∼ 0 . 08 , indicating that the role of lensing is minimal. The systems in the fourth panel have R$_{E}$/R$_{WD}$ < 0 . 4 . They each have a high probability of generating transits, but lensing effects will be more subtle and difficult to detect. Table 1 summarizes the numerical results for these four categories across simulations. General Features: We note that, although the majority of white dwarfs orbiting main- sequence stars lie in larger orbits, and are descended from progenitors that did not interact, white dwarfs in wide orbits contribute little to either transits or lensing events. We expect only roughly 2 Kepler lensing events to be generated by white dwarfs that are the remnants of stars that do not fill their Roche lobes. The lensing signal will be dominated by white dwarfs formed in mass transfer binaries. Of these, common envelope survivors seem likely to dominate. This is because, for any given orbital separation, white dwarfs emerging from a common envelope tend to have higher mass. We note that we also kept track of low- luminosity companions to monitored main-sequence. We compute that those with orbital periods larger than ∼ 4 days producing transits of Kepler -monitored stars may be ∼ 20 times less common than the white dwarfs which transit Kepler targets (see Figure 5). These will produce transits with no evidence of lensing. Magnification without Transits: The disk of a small object must directly overlap the disk of its stellar companion to decrease the amount of light we receive from it. Detectable lensing can occur, however, even without overlap between the object and its companion. Thus, the cross section for lensing events is higher, and the lensing events caused by transiting white dwarfs will be supplemented by lensing events caused by the dwarfs making more distant approaches. The rate of pure lensing events depends on finite source size effects, so it must be computed in each case. The enhancement of a factor will be modest. For objects more compact and more massive than white dwarfs, lensing is by far the dominant effect, and – 22 –