Search results
Results from the WOW.Com Content Network
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]
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 ...
The white dwarf PHL 5038A was discovered in 2006 in data from the Sloan Digital Sky Survey [3] and the brown dwarf companion was discovered in 2009 from UKIDSS infrared excess and confirmed with Gemini North to be a spacially resolved binary. [4] It was only the fourth known brown dwarf to orbit a white dwarf at the time.
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).
They are created as a result of supernovas and gravitational collapse, [2] ... Binary with a white dwarf PSR J0952–0607: Black Widow Pulsar: Sextans: 09h 52m 08.319s:
AM CVn stars with a white-dwarf donor can be formed when a binary consisting of a white dwarf and a low-mass giant evolve through a common-envelope (CE) phase. The outcome of the CE will be a double white-dwarf binary. Through the emission of gravitational radiation, the binary loses angular momentum, which causes
AR Scorpii (AR Sco) is a binary pulsar that consists of a white dwarf and a red dwarf. [3] It is located close to the ecliptic plane in the constellation Scorpius. Parallax measurements made by Gaia put the system at a distance of about 380 light-years (120 parsecs).
Known examples are variations on a binary star : A pulsar–white dwarf system; e.g, PSR B1620−26. A pulsar–neutron star system, e.g, PSR B1913+16. A pulsar and a normal star; e.g, PSR J0045−7319, a system that is composed of a pulsar and main-sequence B star.