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The detection of a dust disc around G29-38 and transits from debris orbitingWD1145+017 confirmed that the photospheric trace metals found in many whitedwarfs arise from the accretion of tidally disrupted planetesimals. Thecomposition of these planetesimals is similar to that of rocky bodies in theinner solar system. Gravitationally scattering planetesimals towards the whitedwarf requires the presence of more massive bodies, yet no planet has so farbeen detected at a white dwarf. Here we report optical spectroscopy of a$\simeq27\,750$K hot white dwarf that is accreting from a circumstellar gaseousdisc composed of hydrogen, oxygen, and sulphur at a rate of$\simeq3.3\times10^9\,\mathrm{g\,s^{-1}}$. The composition of this disc isunlike all other known planetary debris around white dwarfs, but resemblespredictions for the makeup of deeper atmospheric layers of icy giant planets,with H$_2$O and H$_2$S being major constituents. A giant planet orbiting a hotwhite dwarf with a semi-major axis of $\simeq15$ solar radii will undergosignificant evaporation with expected mass loss rates comparable to theaccretion rate onto the white dwarf. The orbit of the planet is most likely theresult of gravitational interactions, indicating the presence of additionalplanets in the system. We infer an occurrence rate of spectroscopicallydetectable giant planets in close orbits around white dwarfs of$\simeq10^{-4}$.

Accretion of a giant planet onto a white dwarf