  Our work examines the detectability of tidally distorted solid exoplanets in
synchronous rotation. Previous work has shown that tidally distorted shapes of
close-in gas giants can give rise to radius underestimates and subsequently
density overestimates for those planets. We examine the assumption that such an
effect is too minimal for rocky exoplanets and find that for smaller M Class
stars there may be an observationally significant tidal distortion effect at
very close-in orbits. We quantify the effect for different stellar types and
planetary properties using some basic assumptions. Finally, we develop a simple
analytic expression to test if there are detectable bulge signatures in the
photometry of a system. We find that close in for smaller M Class stars there
may be an observationally significant signature that may manifest itself in
both in-transit bulge signatures and ellipsoidal variations.
