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Be–white dwarf X-ray binary systems (BeWDs) are a rare type of X-ray binary consisting of a white dwarf that accretes matter from a rapidly-rotating Be star. These systems form through binary evolution where mass transfer spins up the accretor to become a Be star while the donor evolves into a white dwarf. [2]
The highly magnetized white dwarf in the binary system AR Scorpii was identified in 2016 as the first pulsar in which the compact object is a white dwarf instead of a neutron star. [118] A second white dwarf pulsar was discovered in 2023. [119]
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 .
The well-known binary star Sirius, seen here in a Hubble photograph from 2005, with Sirius A in the center, and white dwarf, Sirius B, to the left bottom from it. A binary star or binary star system is a system of two stars that are gravitationally bound to and in orbit around each other.
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 [6] [7] First singular white dwarf with a transiting object WD 1145+017: 2015 Known object is a disintegrating planetesimal, most likely an asteroid. [8] First white dwarf that is ...
This collision can leave behind a close binary system of two white dwarfs. Their orbit decays and they merge through their shared envelope. [ 27 ] A study based on SDSS spectra found 15 double systems of the 4,000 white dwarfs tested, implying a double white dwarf merger every 100 years in the Milky Way: this rate matches the number of Type Ia ...
White dwarfs are among the most compact objects in the cosmos, though not as dense as a black hole. Stars with up to eight times the mass of our sun appear destined to end up as a white dwarf.
HM Cancri (also known as HM Cnc or RX J0806.3+1527) is a binary star system about 1,600 light-years (490 pc; 1.5 × 10 16 km) away. [2] It comprises two dense white dwarfs orbiting each other once every 5.4 minutes, at an estimated distance of only 80,000 kilometres (50,000 miles) apart (about 1/5 the distance between the Earth and the Moon).