The three-body problem is famously chaotic, with no closed-form analytical solutions. However, hierarchical systems of three or more bodies can be stable over indefinite timescales. A system is considered hierarchical if the bodies can be divided into separate two-body orbits with distinct time and length scales, such that one orbit is only mildly affected by the gravitation of the other bodies. Previous work has mapped the stability of such systems at varying resolutions over a limited range of parameters, and attempts have been made to derive analytic and semi-analytic stability boundary fits to explain the observed phenomena. Certain regimes are understood relatively well. However, there are large regions of the parameter space which remain unmapped, and for which the stability boundary is poorly understood. We present a comprehensive numerical study of the stability boundary of hierarchical triples over a range of initial parameters. Specifically, we consider the mass ratio of the inner binary to the outer third body (
$q_\mathrm{out}$
), mutual inclination (i), initial mean anomaly and eccentricity of both the inner and outer binaries (
$e_\mathrm{in}$
and
$e_\mathrm{out}$
respectively). We fit the dependence of the stability boundary on
$q_\mathrm{ out}$
as a threshold on the ratio of the inner binary’s semi-major axis to the outer binary’s pericentre separation
$a_\mathrm{in}/R_\mathrm{p, out} \leq 10^{-0.6 + 0.04q_\mathrm{out}}q_\mathrm{out}^{0.32+0.1q_\mathrm{out}}$
for coplanar prograde systems. We develop an additional factor to account for mutual inclination. The resulting fit predicts the stability of
$10^4$
orbits randomly initialised close to the stability boundary with
$87.7\%$
accuracy.