Search results
Results from the WOW.Com Content Network
SDSS 1557 (SDSS J155720.77+091624.6, WD 1554+094) is a binary system composed of a white dwarf and a brown dwarf.The system is surrounded by a circumbinary debris disk.The debris disk was formed when a minor planet was tidally disrupted around the white dwarf in the past.
WD J0651+2844 is a white dwarf binary star system composed of two white dwarfs. [2] They are approximately 120,000 km apart and complete an orbit around their barycenter in less than 13 minutes. [1] This produces an eclipse every 6 minutes. This makes it possible to gather enough data to produce extremely accurate predictions of each future ...
White dwarfs can also exist as binaries or multiple star systems that only consist of white dwarfs. An example of a resolved triple white dwarf system is WD J1953-1019, discovered with Gaia DR2 data. [211] One interesting field is the study of remnant planetary systems around white dwarfs.
This is the first triple system of white dwarfs to be resolved. [ 3 ] [ 1 ] The three white dwarfs have an atmosphere of pure hydrogen and a mass of about 0.6 times that of the Sun. The system consists of a central pair, WD J1953−1019 BC, and a distant companion, WD J1953−1019 A. WD J1953−1019 B and C correspond to the sources Gaia DR2 ...
The model developed to explain the observations was that AM Canum Venaticorum is a binary system consisting of a pair of white dwarfs in a close orbit. The primary is a more massive white dwarf composed of carbon / oxygen , whereas the secondary is a less massive white dwarf made of helium , with no hydrogen but traces of heavier elements. [ 2 ]
This system consists of two white dwarfs orbiting about each other once every 39 minutes. It was one of the shortest-period detached binary white dwarf systems known in 2011 [ 2 ] They are separated from each other by only 32% of the radius of the Sun , so that each dwarf is tidally distorting the other.
A symbiotic binary is a type of binary star system, often simply called a symbiotic star. They usually contain a white dwarf with a companion red giant . The cool giant star loses material via Roche lobe overflow or through its stellar wind , which flows onto the hot compact star, usually via an accretion disk .
Van Maanen's star is also the nearest solitary white dwarf [4] First white dwarf with a planet WD B1620−26: 2003 PSR B1620-26 b (planet) This planet is a circumbinary planet, which circles both stars in the PSR B1620-26 system [5] [6] First singular white dwarf with a planet WD 1145+017: 2015 WD 1145+017 b: Planet is extremely small and is ...