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It is shown herein that planets with eccentric orbits are more likely totransit than circularly orbiting planets with the same semimajor axis by afactor of (1-e^2)^{-1}. If the orbital parameters of discovered transitingplanets are known, as from follow-up radial velocity observations, then thetransit-detected planet population is easily debiased of this effect. Theduration of a planet's transit depends upon of its eccentricity and longitudeof periastron; transits near periastron are shorter, and those near apoastronlast longer, for a given impact parameter. If fitting for the stellar radiuswith the other transit parameters, this effect causes a systematic error in theresulting measurements. If the stellar radius is instead held fixed at a valuemeasured independently, then it is possible to place a lower limit on theplanet's eccentricity using photometry alone. Orbital accelerations cause adifference in the planet's ingress and egress durations that lead to anasymmetry in the transit lightcurve that could be used along with the transitvelocity measurement to uniquely measure the planet's eccentricity andlongitude of periapsis. However, the effect is too small to be measured withcurrent technology. The habitability of transiting terrestrial planets found byKepler depends on those planets' orbital eccentricities. While Kepler will beable to place lower limits on those planets' orbital eccentricity, the actualvalue for any given planet will likely remain unknown.

Effects of Orbital Eccentricity on Extrasolar Planet Transit Detection and Lightcurves