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Van Maanen 2, or van Maanen's Star, is the closest known solitary white dwarf to the Solar System. It is a dense, compact stellar remnant no longer generating energy and has equivalent to about 68% of the Sun's mass but only 1% of its radius. [ 9 ]
A white dwarf can also be cannibalized or evaporated by a companion star, causing the white dwarf to lose so much mass that it becomes a planetary mass object. The resultant object, orbiting the former companion, now host star, could be a helium planet or diamond planet. [150] [151] [152]
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. [14] ZTF J1901+1458: 1,809 Currently the most massive white dwarf known. [15] Janus: 3,400 A white dwarf with a side of hydrogen and another side of helium. [16] Wolf 1130 ...
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 ...
G 240-72 has mass 0.81 Solar masses [2] and surface gravity 10 8.36 (2.29 · 10 8) cm·s −2, [2] or approximately 234 000 of Earth's, corresponding to a radius 6850 km, or 107% of Earth's. This white dwarf has relatively low temperature 5590 K [2] (slightly cooler than the Sun), and old cooling age, i. e. age as degenerate star (not counting ...
The Hertzsprung–Russell diagram showing the location of main sequence dwarf stars and white dwarfs. A dwarf star is a star of relatively small size and low luminosity. Most main sequence stars are dwarf stars. The meaning of the word "dwarf" was later extended to some star-sized objects that are not stars, and compact stellar remnants that ...
Gliese 440 is the remnant of a massive B-type star that had an estimated 4.4 solar masses. [23] [24] While it was on the main sequence, it probably was a spectral class B star (in the range B4–B9). [23] Most of the star's original mass was shed after it passed into the asymptotic giant branch stage, just prior to becoming a white dwarf.
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. [ 7 ] GD 358 was discovered during the 1958–1970 Lowell Observatory survey for high proper motion stars in the Northern Hemisphere . [ 8 ]