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The visible radiation emitted by white dwarfs varies over a wide color range, from the whitish-blue color of an O-, B- or A-type main sequence star to the yellow-orange of a late K- or early M-type star. [67]
About 6% of white dwarfs show infrared excess due to a disk around a white dwarf. [68] In the past only a relative small sample of white dwarf disks was known. [69] Due to advances in white dwarf detection (e.g. with Gaia or LAMOST) and improvement of WISE infrared catalogs with unWISE/CatWISE, the number has increased to hundreds of candidates.
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: 2015 Known object is a disintegrating ...
Scientists have detected emanating from the nucleus of a galaxy relatively close to our Milky Way flashes of X-rays gradually increasing in frequency that seem to be coming from a white dwarf - a ...
The white dwarf cooling anomaly is an additional cooling delay that has been observed for ultramassive forms of these compact stellar remnants. [ 1 ] [ 2 ] As a white dwarf cools, crystallization of the interior releases energy, slowing the cooling rate.
The Eskimo Nebula is illuminated by a white dwarf at its center. The stars called white or degenerate dwarfs are made up mainly of degenerate matter; typically carbon and oxygen nuclei in a sea of degenerate electrons. White dwarfs arise from the cores of main-sequence stars and are therefore very hot when
White dwarfs are the remnants of low-mass stars which, if they form a binary system with another star, can cause large stellar explosions known as type Ia supernovae. The normal route by which this happens involves a white dwarf drawing material off a main sequence or red giant star to form an accretion disc.
Companion is a white dwarf which is one of the most massive at 1.319 M ☉ [24] PSR B1957+20: 1.81 ± 0.17: 6,500: Substellar object: Rate of advance of periastron. Prototype star of black widow pulsars. [25] [26] [27] SWIFT J1756.9-2508: 1.8 ± 0.4: 26,100 Substellar object: Hosts one planet, it is notable for orbiting its star in 54 minutes ...