The Binary White Dwarf LHS 3236
Abstract
The white dwarf LHS 3236 (WD1639+153) is shown to be a double-degenerate binary, with each component having a high mass. Astrometry at the U.S. Naval Observatory gives a parallax and distance of 30.86 +/- 0.25 pc and a tangential velocity of 98 km/s, and reveals binary orbital motion. The orbital parameters are determined from astrometry of the photocenter over more than three orbits of the 4.0-year period. High-resolution imaging at the Keck Observatory resolves the pair with a separation of 31 and 124 mas at two epochs. Optical and near-IR photometry give a set of possible binary components. Consistency of all data indicates that the binary is a pair of DA stars with temperatures near 8000 and 7400 K and with masses of 0.93 and 0.91 M_solar; also possible, is a DA primary and a helium DC secondary with temperatures near 8800 and 6000 K and with masses of 0.98 and 0.69 M_solar. In either case, the cooling ages of the stars are ~3 Gyr and the total ages are <4 Gyr. The combined mass of the binary (1.66--1.84 M_solar) is well above the Chandrasekhar limit; however, the timescale for coalescence is long.
Cite
@article{arxiv.1309.1173,
title = {The Binary White Dwarf LHS 3236},
author = {Hugh Harris and Conard Dahn and Trent Dupuy and Blaise Canzian and Harry Guetter and William Hartkopf and Michael Ireland and Sandy Leggett and Stephen Levine and Michael Liu and Christian Luginbuhl and Alice Monet and Ronald Stone and John Subasavage and Trudy Tilleman and Richard Walker},
journal= {arXiv preprint arXiv:1309.1173},
year = {2015}
}
Comments
Accepted for the Astrophysical Journal