A near-infrared spectroscopic detection of the brown dwarf in the post common envelope binary WD0137-349

Details A near-infrared spectroscopic detection of the brown dwarf in the post common envelope binary WD0137-349 A near-infrared spectroscopic detection of the brown dwarf in the post common envelope binary WD0137-349

2006-09-13

arxiv.org/abs/astro-ph/0609366v1

Mon.Not.Roy.Astron.Soc.Lett. 373 (2006) L55-L59

Astronomy and Astrophysics

Astrophysics

Accepted for publication in MNRAS

Scientific paper

10.1111/j.1745-3933.2006.00242.x

We present a near-infrared spectrum of the close, detached white dwarf + brown dwarf binary WD0137-349 (Maxted et al 2006), that directly reveals the substellar companion through an excess of flux longwards of 1.95 microns. We best match the data with a white dwarf + L8 composite model. For ages ~1 Gyr, the spectral type of the cool secondary is in agreement with the mass determined by Maxted et al. (2006) from radial velocity measurements (0.053 +/- 0.006Msun), and supports an evolutionary scenario in which the brown dwarf survived a previous phase of common envelope evolution which resulted in the formation of this close binary. The brown dwarf is the lowest mass companion to a white dwarf yet found, and the lowest mass object known to have survived a common envelope phase. At 1300 < T < 1400K WD0137-349B is also the coolest known companion to a white dwarf. At a separation a = 0.65Rsun the hemisphere of the brown dwarf facing the 16,500K white dwarf is being heated through irradiation. We discuss the possible effects of this additional heating, with particular relevance to those other close binaries with substellar companions, the hot Jupiters. We propose future observations to investigate the likely temperature differences between the ``day'' and ``night'' sides of the brown dwarf.

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