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Sirius B, which is a white dwarf, can be seen as a faint point of light to the lower of the much brighter Sirius A. A white dwarf is a stellar core remnant composed mostly of electron-degenerate matter. A white dwarf is very dense: in an Earth sized volume, it packs a mass that is comparable to the Sun.
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. However, the cooling rates modelled on this crystal formation process do not always match that ...
About 97% of all stars are destined to become white dwarfs when they die," Caiazzo said. "Our sun, for example, is currently burning hydrogen into helium in its core.
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 ...
This white dwarf started its life as a star about twice the sun's mass, living a lifespan of perhaps 1.2 billion years before entering its death throes. Many white dwarfs have a debris disk ...
The supposed planetesimal, WD 1145+017 b, [13] with a 4.5 hour orbit, is being ripped apart by the star and is a remnant of the former planetary system that the star hosted before becoming a white dwarf. [8] [9] It is the first observation of a planetary object being shredded by a white dwarf. Several other large pieces have been seen in orbit ...
The white dwarf has a radius of 0.011 R ☉, which is about 1.2 times the radius of the earth. Because white dwarfs are such dense objects, LSPM J0207 has a mass of about 0.69 M ☉ . The presence of the Paschen Beta-Line in a near- infrared spectrum from the Keck telescope helped to determine that the atmosphere of LSPM J0207 is dominated by ...
In a binary system consisting of a white dwarf and a companion star, the white dwarf strips away material from its companion. Normally the white dwarf would eventually reach a critical mass, and fusion reactions would make it explode and completely dissipate it, but in a Type Iax supernova, only a part of the dwarf's mass is lost. [8]