The Binary White Dwarf LHS 3236

TL;DR

This paper characterizes the double-degenerate binary white dwarf LHS 3236, determining its orbital parameters, component masses, and ages, and discusses its potential as a supernova progenitor.

Contribution

It provides detailed astrometric, imaging, and photometric analysis of LHS 3236, revealing its binary nature, component properties, and implications for supernova progenitors.

Findings

Binary has a 4-year orbital period.

Component masses are approximately 0.91-0.93 and 0.69-0.98 solar masses.

Total mass exceeds the Chandrasekhar limit, but coalescence timescale is long.

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.