WD J0914+1914


WD J0914+1914 is the first single white dwarf star found to have a giant planet orbiting it. Evidence of the giant planet was discovered by a team of astronomers from the UK, Chile and Germany.
The system was initially identified as a cataclysmic variable on the basis of weak H-alpha emissions in the spectrum by the Sloan Digital Sky Survey. After closer inspection the team of astronomers discovered oxygen and sulfur lines in the SDSS spectra. The team then obtained spectroscopic follow-up observations with X-Shooter on ESO's Very Large Telescope. The spectra confirmed the previous observations by SDSS and found additional lines.
Dusty and gaseous debris disks around white dwarfs are known, but they are dominated by Calcium lines and no previous disk around a white dwarf showed Hα emission. All previous disks around white dwarfs originate from rocky planetary bodies. The size of the disk around WD J0914+1914 was measured with the help of Doppler-broadbanded emission lines. The disk around the white dwarf is too large to be formed by a small minor planet, which was tidally disrupted inside the Roche Radius. The team was also able to exclude accretion of material from a companion star or brown dwarf.
The most plausible explanation is an evaporating giant planet, orbiting close to the white dwarf. The atmosphere of the planet is evaporated by the strong ultraviolet radiation of the hot white dwarf. The planet is likely located at a distance of 15 solar radii from the white dwarf and orbits the white dwarf in 10 days. The composition of the accreted material show similarity of the deeper layers of the ice giants in the solar system. The team estimated that the planet around WD J0914+1914 will lose about 0.04 Neptune masses and thus this process will not significantly change the structure of the planet.