In 19th European Workshop on White Dwarfs, Astronomical Society of the Pacific Conference Series, Vol. Model atmosphere analysis of the magnetic field in cool, hydrogen-line (DA) white dwarfs. Spectrophotometric analysis of magnetic white dwarf - I. The evolution of ultra-massive white dwarfs. The Swift Ultra-Violet/Optical Telescope. An isolated white dwarf with a 70 s spin period. A highly magnetized and rapidly rotating white dwarf as small as the Moon. White dwarf rotation as a function of mass and a dichotomy of mode line widths: Kepler observations of 27 pulsating DA white dwarfs through K2 campaign 8. The Keck Low-resolution Imaging Spectrometer. HiPERCAM: a quintuple-beam, high-speed optical imager on the 10.4-m Gran Telescopio Canarias. CHIMERA: a wide-field, multi-colour, high-speed photometer at the prime focus of the Hale telescope. The Zwicky Transient Facility: system overview, performance, and first results. Discovery of spectroscopic variations in the DAB white dwarf GD 323. From hydrogen to helium: the spectral evolution of white dwarfs as evidence for convective mixing. On the evolution of magnetic white dwarfs. Suppression of cooling by strong magnetic fields in white dwarf stars. A detailed model atmosphere analysis of hot white dwarfs from SDSS DR12. On the spectral evolution of hot white dwarf stars. Hot DB white dwarfs from the Sloan Digital Sky Survey. How much hydrogen is there in a white dwarf? Astrophys. Temperatures for hot and pulsating DB white dwarfs obtained with the IUE Observatory. The Palomar–Green catalog of ultraviolet-excess stellar objects. In IAU Colloquium 95: Second Conference on Faint Blue Stars (eds Philip, A. Recent advances in the theory of white dwarf spectral evolution. Diffusion in white dwarfs: new results and comparative study. Paquette, C., Pelletier, C., Fontaine, G. White Dwarfs (North-Holland Publishing Co., 1958). This class of white dwarfs could help shed light on the physical mechanisms behind the spectral evolution of white dwarfs. 12), a white dwarf that shows similar but much more subtle variations. ZTF J203349.8+322901.1 might be the most extreme member of a class of magnetic, transitioning white dwarfs-together with GD 323 (ref. This peculiar nature is probably caused by the presence of a small magnetic field, which creates an inhomogeneity in temperature, pressure or mixing strength over the surface 9, 10, 11. Here we report observations of ZTF J203349.8+322901.1, a transitioning white dwarf with two faces: one side of its atmosphere is dominated by hydrogen and the other one by helium. Several mechanisms compete with gravitational settling to change a white dwarf’s surface composition as it cools 3, and the fraction of white dwarfs with helium atmospheres is known to increase by a factor of about 2.5 below a temperature of about 30,000 kelvin 4, 5, 6, 7, 8 therefore, some white dwarfs that appear to have hydrogen-dominated atmospheres above 30,000 kelvin are bound to transition to be helium-dominated as they cool below it. In the resulting strong gravity, heavy elements sink towards the centre and the upper layer of the atmosphere contains only the lightest element present, usually hydrogen or helium 1, 2. White dwarfs, the extremely dense remnants left behind by most stars after their death, are characterized by a mass comparable to that of the Sun compressed into the size of an Earth-like planet. Nature volume 620, pages 61–66 ( 2023) Cite this article A rotating white dwarf shows different compositions on its opposite faces
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