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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 ...
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]
The white dwarf existed for 10.21 ±0.22 Gyrs, meaning the total age is 10.7 ±0.3 Gyrs. [1] Cold white dwarfs are often strongly affected by collision induced absorption (CIA) of hydrogen. This can lead to faint optical red and infrared brightness. These white dwarfs are also called IR-faint white dwarfs. WD J2147–4035 is however very red (r ...
First solitary white dwarf Van Maanen 2: 1917 Van Maanen's star is also the nearest solitary white dwarf [5] 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 ...
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. Symbiotic binaries are of particular interest to astronomers as they can be used to learn about stellar evolution.
[4] [3] Earlier mass ratios hinted at a low mass donor and Neustroev & Mäntynen were able to narrow down the mass of the white dwarf to 0.85±0.04 M ☉ and the mass of the donor to 0.051±0.006 M ☉ (53.4±6.3 M J), making the donor a brown dwarf. BW Sculptoris is a candidate period bouncer. This is an evolutionary stage of a cataclysmic ...
PSR J0348+0432 is a pulsar–white dwarf binary system in the constellation Taurus.It was discovered in 2007 with the National Radio Astronomy Observatory's Robert C. Byrd Green Bank Telescope in a drift-scan survey.
One of the currently known binaries that LISA will be able to resolve is the white dwarf binary ZTF J1539+5027 with a period of 6.91 minutes, the second shortest period binary white dwarf pair discovered to date. [47] [48]