  The observed properties of transiting exoplanets are an exceptionally rich
source of information that allows us to understand and characterize their
physical properties. Unfortunately, only a relatively small fraction of the
known exoplanets discovered using the radial velocity technique are known to
transit their host, due to the stringent orbital geometry requirements. For
each target, the transit probability and predicted transit time can be
calculated to great accuracy with refinement of the orbital parameters.
However, the transit probability of short period and eccentric orbits can have
a reasonable time dependence due to the effects of apsidal and nodal
precession, thus altering their transit potential and predicted transit time.
Here we investigate the magnitude of these precession effects on transit
probabilities and apply this to the known radial velocity exoplanets. We assess
the refinement of orbital parameters as a path to measuring these precessions
and cyclic transit probabilities.
