  For the majority of short period exoplanets transiting massive stars with
radiative envelopes, the spin angular momentum of the host star is greater than
the planetary orbital angular momentum. In this case, the orbits of the planets
will undergo nodal precession, which can significantly impact the probability
that the planets transit their parent star. In particular, for some
combinations of the spin-orbit angle $\psi$ and the inclination of the stellar
spin $i_*$, all such planets will eventually transit at some point over the
duration of their precession period. Thus, as the time over which the sky has
been monitored for transiting planets increases, the frequency of planets with
detectable transits will increase, potentially leading to biased estimates of
exoplanet occurrence rates, especially orbiting more massive stars.
Furthermore, due to the dependence of the precession period on orbital
parameters such as spin-orbit misalignment, the observed distributions of such
parameters may also be biased. We derive the transit probability of a given
exoplanet in the presence of nodal precession induced by a rapidly spinning
host star. We find that the effect of nodal precession has already started to
become relevant for some short-period planets, i.e., Hot Jupiters, orbiting
massive stars, by increasing transit probabilities by of order a few percent
for such systems within the original $Kepler$ field. We additionally derive
simple expressions to describe the time evolution of the impact parameter $b$
for applicable systems, which should aid in future investigations of exoplanet
nodal precession and spin-orbit alignment.
