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A white dwarf is a stellar core remnant composed mostly of electron-degenerate matter. A white dwarf is very dense: its mass is comparable to the Sun's, while its volume is comparable to Earth's. No nuclear fusion takes place in a white dwarf. Instead, the light it radiates comes from the residual heat stored in it. [1]
A light curve for ZTF J0139+5245, showing the ZTF red and green band data during the period of the first two observed transit events. Adapted from Vanderbosch et al. [1] The 107.2 day orbital period is shown in purple. The white dwarf has a mass of 0.54 M ☉, a temperature of 10,530 ± 140 K and a log (g) of 7.86 ± 0.06. [1]
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 ...
This includes both red dwarfs and brown dwarfs that are very faint in the visible spectrum. [ 95 ] Brown dwarfs , stars that do not undergo hydrogen fusion , cool as they age and so progress to later spectral types.
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 ...
However, measurements by Adams have been criticized as being too low [15] [16] and these observations are now considered to be measurements of spectra that are unusable because of scattered light from the primary, Sirius A. [16] The first accurate measurement of the gravitational redshift of a white dwarf was done by Popper in 1954, measuring a ...
WD 1856+534 is a white dwarf located in the constellation of Draco.At a distance of about 25 parsecs (80 ly) from Earth, it is the outer component of a visual triple star system consisting of an inner pair of red dwarf stars, named G 229-20.
It has a mass of 84 to 87 M J, making VVV 1256−62B likely a red dwarf star. [14] The subdwarf Wolf 1130C (sdT8) is the companion of an old subdwarf-white dwarf binary, which is estimated to be older than 10 billion years. It has a mass of 44.9 M J, making it a brown dwarf.