  The orbit of a planet is surrounded by a chaotic zone wherein nearby
particles' orbits are chaotic and unstable. Wisdom (1980) showed that the chaos
is driven by the overlap of mean motion resonances which occurs within a
distance (da/a)_chaos = 1.3 mu^2/7 of the planet's orbit. However, the width of
mean motion resonances grows with the particles' eccentricity, which will
increase the width of the chaotic zone at higher eccentricities. Here we
investigate the width of the chaotic zone using the iterated encounter map and
N-body integrations. We find that the classical prescription works well for
particles on low-eccentricity orbits. However, above a critical eccentricity,
dependent upon the mass of the planet, the width of the chaotic zone increases
with eccentricity. An extension of Wisdom's analytical arguments then shows
that, above the critical eccentricity, the chaotic zone width is given by
(da/a)_chaos = 1.8 e^1/5 mu^1/5, which agrees well with the encounter map
results. The critical eccentricity is given by e_cr = 0.21 mu^3/7. This
extended chaotic zone results in a larger cleared region when a planet sculpts
the inner edge of a debris disc comprised of eccentric planetesimals. Hence,
the planet mass estimated from the classical chaotic zone may be erroneous. We
apply this result to the HR8799 system, showing that the masses of HR8799b
inferred from the truncation of the disc may vary by up to 50% depending on the
disc particles' eccentricities. With a disc edge at 90AU, the necessary mass of
planet b to cause the truncation would be 8-10 Jovian masses if the disc
particles have low eccentricities (<0.02), but only 4-8 Jovian masses if the
disc particles have higher eccentricities. Our result also has implications for
the ability of a planet to feed material into an inner system, a process which
may explain metal pollution in White Dwarf atmospheres.
