Wolf 1346
Wolf 1346, otherwise known as HD 340611 and WD 2032+248, is a star in the northern constellation of Vulpecula. With an apparent magnitude of 11.546, it is too faint to be seen by the naked eye but can be observed using a telescope with an aperture of or larger. It is located at a distance of approximately according to Gaia EDR3 parallax measurements, and is receding from the Sun at a heliocentric radial velocity of +71.0 km/s.
Properties
This is a young, non-magnetic white dwarf with an age of 60 million years. It is a little less than two-thirds the mass of the Sun and just 1.4% the radius, that is 1.5 times the size of Earth or. With an effective temperature of, it shines with 3.3% of the Sun's luminosity. It belongs to the thin disk of the Milky Way. There is marginal indication that the star is orbited by a binary companion.It has the spectral type DA2.4, indicating that the atmosphere is dominated by hydrogen, which is the only element whose spectral lines show up in the star's visible spectrum. It has been subject to multiple ultraviolet spectroscopic observations. Silicon lines were discovered in 1984 from spectra obtained by the International Ultraviolet Explorer. The abundance of silicon in the photosphere has been measured at log=−7.5 ± 0.2, which, compared to the solar value of log=−4.5, is approximately one thousand times less. This amount is comparable to what is expected from radiative levitation. Carbon, nitrogen, and oxygen are absent in the spectra, consistent with theories of element diffusion. Observations by the Hopkins Ultraviolet Telescope revealed that the Lyman-beta line shows signs of the dihydrogen cation, which, in cooler DA white dwarfs, causes similar signatures in the Lyman-alpha line.