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Eddington predicted that dwarf stars remain in an essentially static position on the main sequence for most of their lives. In the 1930s and 1940s, with an understanding of hydrogen fusion, came an evidence-backed theory of evolution to red giants following which were speculated cases of explosion and implosion of the remnants to white dwarfs.
The Hertzsprung–Russell diagram showing the location of main sequence dwarf stars and white dwarfs. A dwarf star is a star of relatively small size and low luminosity. Most main sequence stars are dwarf stars. The meaning of the word "dwarf" was later extended to some star-sized objects that are not stars, and compact stellar remnants that ...
The white dwarf luminosity function (WDLF) gives the number of white dwarf stars with a given luminosity. As this is determined by the rates at which these stars form and cool, it is of interest for the information it gives about the physics of white dwarf cooling and the age and history of the Galaxy. [3] [4]
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 .
Download as PDF; Printable version; ... White dwarfs (3 C, 167 P) B. Brown dwarfs (5 C, 167 P) R. Red dwarfs (2 C, 13 P) Pages in category "Stars by luminosity class"
G29-38 was shown to radiate substantial emission between 2 and 5 micrometres, far in excess of that expected from extrapolation of the visual and near infrared spectrum of the star. [12] 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 ...
ESO 439-26 was considered the least luminous white dwarf known. [2] [7] Located 140 light years away from the Sun, it is roughly 10 billion years old and has a temperature of 4560 Kelvin. Thus, despite being classified as a "white dwarf", it would actually appear yellowish in color. [8] This finding is however based on a too large parallax.
G 240-72 is the seventh closest white dwarf (after Sirius B, Procyon B, van Maanen's star, Gliese 440, 40 Eridani B and Stein 2051 B). Its trigonometric parallax , as measured by the Gaia space telescope, is 160.9952 ± 0.0119 mas , [ 1 ] corresponding to a distance of 6.2114 parsecs (20.259 light-years ).