  Rings around giant exoplanets (hereafter 'exorings') are still a missing
planetary phenomenon among the vast number of discovered planets. Despite the
fact there exist a large number of methods for identifying and characterizing
these exorings, none of them has been successful to date. Most of those efforts
focus on the photometric signatures produced by rings around transiting
exoplanets; thus, little interest has been intended for the detectable
signatures that non-transiting ringed planets might cause owing to the excess
of scattered starlight from both their atmosphere and the considerably large
surface of their (hypothetical) rings-system. This extra scattering produced by
exorings would occur at an orbital location defined here as the `the summer
solstice' of a stellar light curve. In this letter, we develop a first-order
model to estimate the photometric signatures of non-transiting exorings and
predict their detectability by using present and future facilities. We also
show how, besides the discovery itself, our model can be used to constrain
orbital and physical parameters of planet-rings systems.

Earth and Planetary Astrophysics;Instrumentation and Methods for Astrophysics