  Planets that orbit only one of the stars in stellar binary systems (i.e.,
circumstellar) are dynamically constrained to a limited range of orbital
parameters and thus understanding conditions on their stability is of great
importance in exoplanet searches. We perform $\sim$700 million N-body
simulations to identify how stability regions depend on properties of the
binary, as well as, the starting planetary inclination and mean longitude
relative to the binary orbit. Moreover, we provide grid interpolation maps and
lookup tables for the community to use our results. Through Monte-Carlo methods
we determine that planets with a semimajor axis $a_p$ $\lesssim$8\% of the
binary semimajor axis $a_{bin}$ will likely be stable given the known
distribution of binary star parameters. This estimate varies in the Lidov-Kozai
regime or for retrograde orbits to 4\% or 10\% of $a_{bin}$, respectively. Our
method to quickly determine the circumstellar stability limit is important for
interpreting observations of binaries using direct imaging with JWST,
photometry with TESS, or even astrometry with Gaia.
