– 19 – -2 0 2 4 -6 -4 -2 0 Fig. 5.— Low-mass stellar dwarfs may produce transits that mimic planetary transits. Here we plot the probability of a transit versus the logarithm of the orbital period. The bend at one year corresponds to P$_{orb}$ = τ$_{monitor}$. For shorter orbital periods, the probability falls as 1 /a ; for longer orbital periods the ratio between τ$_{monitor}$/P$_{orb}$ must also be factored in. The presence of low-mass dwarfs with luminosities in the range of 10 − 4 − 10 − 3 times the luminosity of the star monitored by Kepler may be detectable only because they produce detectable transits, and are themselves detectably eclipsed. We kept track of these systems in our simulations. Considering only those with orbital periods greater than 4 days, we found that they should produce transits at ∼ 5% the rate caused by white dwarfs that emerge from common envelopes. The total contribution is likely to be higher.