2019MNRAS.484.2566L

We present new XSHOOTER spectra of NLTT5306, a 0.44 ± 0.04 M_☉ white dwarf in a short period (101 min) binary system with a brown dwarf companion that is likely to have previously undergone common envelope evolution. We have confirmed the presence of H α emission and discovered Na I absorption associated with the white dwarf. These observations are indicative of accretion. Accretion is typically evidenced by high-energy emission in the UV and X-ray regime. However our Swift observations covering the full orbital period in three wavebands (uvw1, uvm2, uvw2) revealed no UV excess or modulation. We used the X-ray non-detection to put an upper limit on the accretion rate of 2 x 10^–15 M_☉ yr^–1. We compare NLTT5306 to similar accreting binaries with brown dwarf donors and suggest the inferred accretion rate could be from wind accretion or accretion from a debris/dust disc. The lack of evidence for a disc implies NLTT5306 is magnetically funnelling a weak wind from a potentially low-gravity brown dwarf. The upper limit on the accretion rate suggests a magnetic field as low as 0.45 kG would be sufficient to achieve this. If confirmed this would constitute the first detection of a brown dwarf wind and could provide useful constraints on mass-loss rates.