  We analyze the potential transit light curve effects due to a Clarke belt of
satellites around an exoplanet. Building on code and analysis from Korpela,
Sallmen, & Leystra Greene (2015), we refine the transit analysis of
Socas-Navarro (2018) by incorporating limb-darkening and taking an
observer-centered approach to examining residuals. These considerations make
Clarke exobelt detectability more difficult than previous estimates. We also
consider practical dynamical issues for exobelts, confirming that synchronously
orbiting belts are dynamically unstable around planets in the habitable zones
of M stars, and determining the maximum quasi-stable belt size in these
situations. Using simulations for both G and M stars, we conclude that to have
an even marginally detectable impact on transit light curves, exobelts must be
substantially denser than previous estimates. We also estimate collision rates
for the required satellite densities assuming random orbits, and find they
would present significant monitoring and guidance challenges. If detectable
belts exist, they would require some (possibly high) degree of ordering to
avoid collisions, and must be actively maintained or they will dissipate on
relatively short astronomical timescales. We conclude that detectable exobelts
are likely to be rare, and have extremely low prospects for detection by
transit monitoring from both current and upcoming missions.
