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First solitary white dwarf Van Maanen 2: 1917 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 ...
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]
G117-B15A [7] is a small, well-observed variable white dwarf star of the DAV, or ZZ Ceti, type in the constellation of Leo Minor. G117-B15A was found to be variable in 1974 by Richer and Ulrych, [8] and this was confirmed in 1976 by McGraw and Robinson. [9] In 1984 it was demonstrated that the star's variability is due to nonradial gravity wave ...
White dwarf effective surface temperatures extend from over 150 000 K [24] to barely under 4000 K. [68] [69] In accordance with the Stefan–Boltzmann law, luminosity increases with increasing surface temperature (proportional to T 4); this surface temperature range corresponds to a luminosity from over 100 times that of the Sun to under 1 ...
Printable version; In other projects ... 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"
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 ).
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 ...