Debris disk

and Hubble images of the disc around AU Microscopii. In 1984 a debris disk was detected around the star Vega using the IRAS satellite. Initially this was believed to be a protoplanetary disk, but it is now known to be a debris disk due to the lack of gas in the disk and the age of the star. The first four debris disks discovered with IRAS are known as the "fabulous four": Vega, Beta Pictoris, Fomalhaut, and Epsilon Eridani. Subsequently, direct images of the Beta Pictoris disk showed irregularities in the dust, which were attributed to gravitational perturbations by an unseen exoplanet. That explanation was confirmed with the 2008 discovery of the exoplanet Beta Pictoris b. Other exoplanet-hosting stars, including the first discovered by direct imaging (HR 8799), are known to also host debris disks. The nearby star 55 Cancri, a system that is also known to contain five planets, also was reported to have a debris disk, but that detection could not be confirmed. Structures in the debris disk around Epsilon Eridani suggest perturbations by a planetary body in orbit around that star, which may be used to constrain the mass and orbit of the planet. On 24 April 2014, NASA reported detecting debris disks in archival images of several young stars, HD 141943 and HD 191089, first viewed between 1999 and 2006 with the Hubble Space Telescope, by using newly improved imaging processes. In 2021, observations of a star, VVV-WIT-08, that became obscured for a period of 200 days may have been the result of a debris disk passing between the star and observers on Earth. Two other stars, Epsilon Aurigae and TYC 2505-672-1, are reported to be eclipsed regularly and it has been determined that the phenomenon is the result of disks orbiting them in varied periods, suggesting that VVV-WIT-08 may be similar and have a much longer orbital period that just has been experienced by observers on Earth. VVV-WIT-08 is ten times the size of the Sun in the constellation of Sagittarius. ==Origin==

detected in HST archival images of young stars, HD 141943 and HD 191089, using improved imaging processes (24 April 2014). Typical debris disks contain small grains 1–100 μm in size. Collisions will grind down these grains to sub-micrometre sizes, which will be removed from the system by radiation pressure from the host star. In very tenuous disks such as the ones in the Solar System, the Poynting–Robertson effect can cause particles to spiral inward instead. Both processes limit the lifetime of the disk to 10 Myr or less. Thus, for a disk to remain intact, a process is needed to continually replenish the disk. This can occur, for example, by means of collisions between larger bodies, followed by a cascade that grinds down the objects to the observed small grains. For collisions to occur in a debris disk, the bodies must be gravitationally perturbed sufficiently to create relatively large collisional velocities. A planetary system around the star can cause such perturbations, as can a binary star companion or the close approach of another star. Furthermore, many debris disks also show structures within the dust (for example, clumps and warps or asymmetries) that point to the presence of one or more exoplanets within the disk. == Extreme debris disks ==

A sub-type of debris disk is the so-called "extreme debris disk" (EDD). This type is defined as exceeding 1% of the luminosity of the star in the infrared. An EDD is surrounded by warm dust (200-600 Kelvin), that orbits the star within a few astronomical units. In other words the dust is present in a region where terrestrial planets form. EDDs are rare and around 24 are known as of 2024. Infrared spectra with Spitzer have shown that the dust is dominated by small particles made up of silicates that have a size between sub-μm and a few μm. EDDs are interpreted to have formed from one or more giant collisions between large planetesimals or planetary bodies. This is different to most debris disks, which are sustained by smaller collisions. EDDs are often transient events, with the dust produced in the event lasting years around the star before radiation pressure blows the small particles away. 2MASS J08090250-4858172 was one of the first such systems with observed infrared variability, showing two giant impact events in 2012 and 2014. In rare cases the dust cloud can orbit in front of the star, causing dips of brightness in the optical. One such system is HD 166191, which shows a star-sized dust cloud transiting in front of the star. Giant impacts are more common in young systems and after around 300 Myrs giant impacts become less common. A few relative old EDDs are also known, reaching up to 5.5 Gyrs. These old EDDs often have a wide, eccentric companion, which might help trigger such giant impact events. ==Known belts==

Belts of dust or debris have been detected around many stars, including the Sun, including the following: The orbital distance of the belt is an estimated mean distance or range, based either on direct measurement from imaging or derived from the temperature of the belt. The Earth has an average distance from the Sun of 1 AU. ==See also==