WD 2359-434 (Gliese 915, LHS 1005, L 362-81) is a nearby degenerate star (white dwarf) of spectral class DAP5.8, the single known component of the system, located in the constellation Phoenix, the nearest star in this constellation.
Currently, the most accurate distance estimate of WD 2359−434 is a trigonometric parallax from Gaia DR3:, corresponding to a distance of, or . WD 2359−434 is the 13th closest white dwarf to the Sun.
WD 2359−434's mass is 0.85 ± 0.01 Solar masses, 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,[1] i.e. mass of one cubic millimetre 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.
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,[2] using Wood model D[3] 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),[3] 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,[4] 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.