1999/06/03 by Hugh Harris, Hugh C. Harris, Conard Dahn +10 · 6 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Binary star #Black dwarf #Blue dwarf #Halo #Spectral line #Star (game theory) #Stars #Stellar, planetary, and galactic studies #White dwarf #astro-ph
paper · pdf · doi:10.1086/307856
23 pages, 6 figures. Accepted for Astrophysical Journal
arxiv created 1999/06/03 · openalex publication_date 1999/10/20 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
The star LHS 3250 is found to be a white dwarf at a distance of 30 pc. Its absolute magnitudes ( M V = 15.72, M bol = 16.2) put it among the least luminous white dwarfs known. Its optical spectrum shows no features, indicating that it has a DC classification, and it shows no detectable polarization, indicating that it does not have a very strong magnetic field. However, its broadband colors show it to have a unique spectral energy distribution, and it stands out from all other stars in BVI and other broadband photometric surveys. We discuss these properties and conclude that LHS 3250 must be an extremely cool white dwarf with strong collision-induced absorption at red-infrared wavelengths from molecular hydrogen, in accord with models for very cool white dwarf atmospheres. If so, it is the first such star known and the first star to provide observational evidence supporting these models. It suggests that other very cool white dwarfs, both halo white dwarfs and the oldest disk white dwarfs, also may have colors affected by similar absorption. The atmospheric composition of LHS 3250 is not known, and therefore its temperature is poorly determined. It is likely to be a helium-core star with a mass 0.3 < M < 0.45 M ☉ and a product of mass transfer in a close binary system. However, until its temperature is better known, its mass and age remain uncertain.