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We present 2D hydrodynamical simulations of hot Jupiters orbiting near theinner edge of protoplanetary discs. We systemically explore how the accretionrate at the inner disc edge is regulated by a giant planet of different mass,orbital separation and eccentricity. We find that a massive (withplanet-to-star mass ratio $\gtrsim 0.003$) eccentric ($e_p\gtrsim 0.1$) planetdrives a pulsed accretion at the inner edge of the disc, modulated at one ortwo times the planet's orbital frequency. The amplitude of accretionvariability generally increases with the planet mass and eccentricity, althoughsome non-monotonic dependences are also possible. Applying our simulationresults to the T Tauri system CI Tau, where a young hot Jupiter candidate hasbeen detected, we show that the observed luminosity variability in this systemcan be explained by pulsed accretion driven by an eccentric giant planet.

Pulsed Disc Accretion Driven by Hot Jupiters