WD 2359−434
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WD 2359-434 (Gliese 915, LHS 1005, L 362-81) is a nearby degenerate star (
white dwarf 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 the Earth's. A white dwarf's faint luminosity comes fro ...
) of spectral class DAP5.8, the single known component of the system, located in the constellation Phoenix, the nearest star in this constellation.


Distance

Currently, the most accurate distance estimate of WD 2359−434 is a
trigonometric parallax Parallax is a displacement or difference in the apparent position of an object viewed along two different sightline, lines of sight and is measured by the angle or semi-angle of inclination between those two lines. Due to perspective (graphica ...
from
Gaia DR3 The ''Gaia'' catalogues are star catalogues created using the results obtained by '' Gaia'' space telescope. The catalogues are released in stages that will contain increasing amounts of information; the early releases also miss some stars, espec ...
: , corresponding to a distance of , or . WD 2359−434 is the 13th closest white dwarf to the Sun.


Physical parameters

WD 2359−434's mass is 0.85 ± 0.01
Solar mass The solar mass () is a standard unit of mass in astronomy, equal to approximately . It is often used to indicate the masses of other stars, as well as stellar clusters, nebulae, galaxies and black holes. It is approximately equal to the mass ...
es, its surface gravity is 108.39 ± 0.01 (2.45 · 108) cm· s−2, or approximately 250,000 of Earth's, corresponding to a radius 6780 km, or 1.06 of Earth's. WD 2359−434 is relatively hot and young white dwarf, its temperature is 8570 ± 50 K; its cooling age, i. e. age as degenerate star (not including lifetime as main sequence star and as giant star) is 1.82 ± 0.06 Gyr. Gliese 518 should appear bluish-white, due temperature, comparable with that of A-type main sequence stars. As all white dwarfs, WD 2359−434 is composed of very dense degenerate matter, its mean density is 1,300,000 g· cm−3,From mass and surface gravity (assuming spherical shape). i.e. mass of one
cubic millimetre The cubic metre (in Commonwealth English and international spelling as used by the International Bureau of Weights and Measures) or cubic meter (in American English) is the unit of volume in the International System of Units (SI). Its symbol is ...
of WD 2359−434 matter is 1.3 kg. Unusually for a white dwarf star, WD 2359-434 has a weak, non-dipole magnetic field of 50,000 - 100,000 Gauss.


Main sequence progenitor properties

As all degenerate stars, WD 2359−434 previously existed initially as main-sequence star and then as giant star, until all the thermonuclear fuel was exhausted, after which WD 2359−434 lost most of its mass. According to the 2010 thesis for the degree of Doctor of Science,Matías Cristóbal Radiszcz Sotomayor, BINARIEDAD ESTELAR Y SUB-ESTELAR EN ENANAS BLANCAS CERCANAS
/ref> using Wood model D initial–final mass relation and WD 2359−434's white dwarf mass value from Holberg et al. 2008, its main sequence progenitor mass was . Using expression for pre-white dwarf lifetime 10 · (MMS/)2.5 (Gyr), was found WD 2359−434 main sequence age 0.07 Gyr. White dwarf mass value from Subasavage et al. 2009, in Wood model D yields MS (main sequence) mass , and MS lifetime 0.11 Gyr, corresponding to B-type main sequence star. According to initial-final mass relation from Weidemann 2000 paper, WD 2359−434's main sequence progenitor should have mass about and lifespan 0.22 Gyr, and, again, should be of B spectral type. There are also other models.


See also

*
List of star systems within 25–30 light-years This is a list of star systems within 25–30 light-years of Earth. See also * List of nearest stars and brown dwarfs * List of star systems within 20–25 light-years * List of star systems within 30-35 light-years * Lists of stars * List of ...


Notes


References

{{DEFAULTSORT:WD 2359-434 White dwarfs Phoenix (constellation) 0915 J00021076-430956