  We carry out hydrodynamical simulations to study the eccentricity growth of a
1-30 Jupiter mass planet located inside the fixed cavity of a protoplanetary
disc. The planet exchanges energy and angular momentum with the disc at
resonant locations, and its eccentricity grows due to Lindblad resonances. We
observe several phases of eccentricity growth where different eccentric
Lindblad resonances dominate from 1:3 up to 3:5. The maximum values of
eccentricity reached in our simulations are 0.65-0.75. We calculate the
eccentricity growth rate for different planet masses and disc parameters and
derive analytical dependencies on these parameters. We observe that the growth
rate is proportional to both the planet's mass and the characteristic disc mass
for a wide range of parameters. In a separate set of simulations, we derived
the width of the 1:3 Lindblad resonance.
