Search results
Results from the WOW.Com Content Network
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 ...
Eddington predicted that dwarf stars remain in an essentially static position on the main sequence for most of their lives. In the 1930s and 1940s, with an understanding of hydrogen fusion, came an evidence-backed theory of evolution to red giants following which were speculated cases of explosion and implosion of the remnants to white dwarfs.
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]
An exoplanet orbits PSR B1620-26 and its white dwarf companion (see below) in a circumbinary orbit. HD 49798: 1,600 White dwarf: One of the smallest white dwarf stars known. [15] ZTF J1901+1458: 1,809 Currently the most massive white dwarf known. [16] Janus: 3,400 A white dwarf with a side of hydrogen and another side of helium. [17] Wolf 1130 ...
Astronomers have discovered a white dwarf star, or the burnt core of a dead star, that has two completely different faces. One is made of hydrogen, while the other is made of helium.
The primary component is a white A-type main sequence star with an apparent magnitude of +7.48. Its furthest companion, HD 74389 B, is a DA-type white dwarf located 20.11 arcseconds west of—at least 190 AU from—HD 74389 A, and has a V magnitude of 14.62.
This dead, dense star remnant is called a white dwarf." As this is the first time scientists have ever seen this "catastrophic destruction" in action, it's a pretty monumental moment for astronomers!
GD 358 is a variable white dwarf star of the DBV type. Like other pulsating white dwarfs, its variability arises from non-radial gravity wave pulsations within the star itself. [8] GD 358 was discovered during the 1958–1970 Lowell Observatory survey for high proper motion stars in the Northern Hemisphere. [9]