Search results
Results from the WOW.Com Content Network
The red giant fills its Roche lobe so that matter is transferred to the white dwarf and accumulates until a nova-like outburst occurs, caused by ignition of thermonuclear fusion. The temperature at maximum is estimated to rise up to 200,000 K, similar to the energy source of novae, but dissimilar to the dwarf novae. The slow luminosity increase ...
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]
That is, the temperature and luminosity of the white dwarf will diminish over time as energy is lost. [6] At a certain point, within the cooling core of a carbon-oxygen white dwarf, electrostatic interactions will start to dominate over thermal motion, and the ions will crystallize into a lattice structure.
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.
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 ...
WD 0343+247 is a white dwarf in the ecliptic constellation of Taurus.It was discovered in 1997 when examination of photographs taken for a survey of brown dwarfs in the Pleiades revealed a faint star with high proper motion.