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The first white dwarf discovered was in the triple star system of 40 Eridani, which contains the relatively bright main sequence star 40 Eridani A, orbited at a distance by the closer binary system of the white dwarf 40 Eridani B and the main sequence red dwarf 40 Eridani C.
In astrophysics, Chandrasekhar's white dwarf equation is an initial value ordinary differential equation introduced by the Indian American astrophysicist Subrahmanyan Chandrasekhar, [1] in his study of the gravitational potential of completely degenerate white dwarf stars.
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 ...
Like other white dwarfs, it is a very dense star: its mass has been estimated to be about 67% of the Sun's, [28] yet it has only 1% of the Sun's radius (1.23 times the Earth's radius). [ 7 ] [ a ] The outer atmosphere has a temperature of approximately 6,110 K , [ 28 ] which is relatively cool for a white dwarf.
BPM 37093 (V886 Centauri) is a variable white dwarf star of the DAV, or ZZ Ceti, type, with a hydrogen atmosphere and an unusually high mass of approximately 1.1 times the Sun's. It is 48 light-years (15 parsecs ) from Earth in the constellation Centaurus and vibrates; these pulsations cause its luminosity to vary .
The surface gravity of a white dwarf is very high, and of a neutron star even higher. A white dwarf's surface gravity is around 100,000 g (10 6 m/s 2) whilst the neutron star's compactness gives it a surface gravity of up to 7 × 10 12 m/s 2 with typical values of order 10 12 m/s 2 (that is more than 10 11 times that of Earth).
A light year is the distance light travels in a year, 5.9 trillion miles (9.5 trillion km). Like all white dwarfs, it is incredibly dense, packing about 70% of the sun's mass into an Earth-sized ...
For reasons that remain unclear, the mass of Procyon B is unusually low for a white dwarf star of its type. [13] With a surface temperature of 7,740 K, it is also much cooler than Sirius B; this is a testament to its lesser mass and greater age. The mass of the progenitor star for Procyon B was about 2.59 +0.22
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