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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).
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.
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 .
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 disintegrating. First white dwarf that is a pulsar: AR Scorpii A ...
Although the white dwarf shows evidence of accretion in the past, at present it is not accreting significantly, and the system is powered by the spin-down of the white dwarf. [7] [5] The white dwarf's rotation will slow down on a timescale of 10 7 years. [5] It has a radius of about 7 × 10 3 km, [5] about the same size as Earth.
An intermediate-mass binary pulsar (IMBP) is a pulsar-white dwarf binary system with a relatively long spin period of around 10–200 ms consisting of a white dwarf with a relatively high mass of approximately . [7] The spin periods, magnetic field strengths, and orbital eccentricities of IMBPs are significantly larger than those of low mass binary pulsars (LMBPs). [7]
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KPD 1930+2752 is a binary star system including a subdwarf B star and a probable white dwarf with relatively high mass. [6] Due to the nature of this astronomical system, it seems like a likely candidate for a potential type Ia supernova, a type of supernova which occurs when a white dwarf star takes on enough matter to approach the Chandrasekhar limit, the point at which electron degeneracy ...