its atmosphere, but van Maanen misclassified it as the faintest F-type star based on the calcium H- and K-lines. The following heavy elements were discovered in the atmosphere of white dwarfs: Ca, Mg, Fe, Na, Si, Cr, C, O, Al?, Sc, Ti, V, Mn, Co, Ni, Cu, Sr, S, P, N, Li, K, Be. The nitrogen in white dwarfs is thought to come from nitrogen-ice of extrasolar Kuiper Belt objects, the lithium is thought to come from accreted crust material and the beryllium is thought to come from exomoons. A less common observable evidence is infrared excess due to a flat and optically thick debris disk, which is found in around 1–4% of white dwarfs. The first white dwarf with infrared excess was discovered by Zuckerman&Becklin in 1987 in the near-infrared around Giclas 29-38 and later confirmed as a debris disk. White dwarfs hotter than 27,000 K sublimate all the dust formed by tidally disrupting a rocky body, preventing the formation of a debris disk. In colder white dwarfs, a rocky body might be tidally disrupted near the Roche radius and forced into a circular orbit by the Poynting–Robertson drag, which is stronger for less massive white dwarfs. The Poynting–Robertson drag will also cause the dust to orbit closer and closer towards the white dwarf, until it will eventually sublimate and the disk will disappear. A debris disk will have a lifetime of around a few million years for white dwarfs hotter than 10,000 K. Colder white dwarfs can have disk-lifetimes of a few 10 million years, which is enough time to tidally disrupt a second rocky body and forming a second disk around a white dwarf, such as the two rings around LSPM J0207+3331. The least common observable evidence of planetary systems are detected major or minor planets. Only a handful giant planets and a handful of minor planets are known around white dwarfs. It is a growing list with discoveries of around 6 exoplanets expected with Gaia and 4 exoplanets with JWST.Infrared spectroscopic observations made by NASA's Spitzer Space Telescope of the central star of the Helix Nebula suggest the presence of a dust cloud, which may be caused by cometary collisions. It is possible that infalling material from this may cause X-ray emission from the central star. Similarly, observations made in 2004 indicated the presence of a dust cloud around the young (estimated to have formed from