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For extrasolar planets with orbital periods, P>10 days, radial velocitysurveys find non-circular orbital eccentricities are common, <e>~0.3. Futuresurveys for extrasolar planets using the transit technique will also havesensitivity to detect these longer period planets. Orbital eccentricity affectsthe detection of extrasolar planets using the transit technique in two opposingways: an enhancement in the probability for the planet to transit nearpericenter and a reduction in the detectability of the transit due to a shortertransit duration. For an eccentricity distribution matching the currently knownextrasolar planets with P>10 day, the probability for the planet to transit is~1.25 times higher than the equivalent circular orbit and the average transitduration is ~0.88 times shorter than the equivalent circular orbit. These twoopposing effects nearly cancel for an idealized field transit survey withindependent photometric measurements that are dominated by Poisson noise. Thenet effect is a modest ~4% increase in the transiting planet yield compared toassuming all planets have circular orbits. When intrinsic variability of thestar or correlated photometric measurements are the dominant source of noise,the transit detectability is independent of the transit duration. In this casethe transit yield is ~25% higher than that predicted under the assumption ofcircular orbits. Since the Kepler search for Earth-sized planets in thehabitable zone of a Solar-type star is limited by intrinsic variability, theKepler mission is expected to have a ~25% higher planet yield than thatpredicted for circular orbits if the Earth-sized planets have an orbitaleccentricity distribution similar to the currently known Jupiter-mass planets.

Impact of Orbital Eccentricity on the Detection of Transiting Extrasolar Planets