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White dwarf - Wikipedia
The white dwarf has a mass of 0.6 M ☉, radius of 0.012 R ☉ (1.34 R 🜨) and a temperature of 15,020 K, typical for white dwarf stars. It has been a white dwarf for 224 million years. [6] [10] The star's spectrum includes strong absorption lines due to magnesium, aluminium, silicon, calcium, iron and nickel.
GD 356 is a white dwarf in the constellation of Draco showing an unusual emission of circular polarised light. The star is 65 light years from earth. [4] The class of this white dwarf is DA e meaning that it has a cool helium rich atmosphere. [5] This star exhibits emission lines showing the Zeeman effect in the hydrogen Balmer spectrum. [5]
DAO – a hydrogen- and helium-rich white dwarf displaying ionized helium lines; DAZ – a hydrogen-rich metallic white dwarf; DBZ – a helium-rich metallic white dwarf; A different set of spectral peculiarity symbols are used for white dwarfs than for other types of stars: [121]
White light is dispersed by a glass prism into the colors of the visible spectrum. The visible spectrum is the band of the electromagnetic spectrum that is visible to the human eye. Electromagnetic radiation in this range of wavelengths is called visible light (or simply light).
When white sunlight enters snow, very little of the spectrum is absorbed; almost all of the light is reflected or scattered by the air and water molecules, so the snow appears to be the color of sunlight, white. Sometimes the light bounces around inside the ice crystals before being scattered, making the snow seem to sparkle.
A pulsating white dwarf is a white dwarf star whose luminosity varies due to non-radial gravity wave pulsations within itself. Known types of pulsating white dwarfs include DAV, or ZZ Ceti, stars, with hydrogen-dominated atmospheres and the spectral type DA; [1] DBV, or V777 Her, stars, with helium-dominated atmospheres and the spectral type DB; [2] and GW Vir stars, with atmospheres dominated ...
Like other young, hot white dwarfs, G29-38 is thought to have formed relatively recently (600 million years ago) from its AGB progenitor, and therefore the excess was naturally explained by emission from a Jupiter-like brown dwarf with a temperature of 1200 K and a radius of 0.15 solar radius.