  We present new optical and near-infrared spectra of WD0137-349; a close white
dwarf - brown dwarf non-interacting binary system with a period of $\approx$114
minutes. We have confirmed the presence of H$\alpha$ emission and discovered
He, Na, Mg, Si, K, Ca, Ti, and Fe emission lines originating from the brown
dwarf atmosphere. This is the first brown dwarf atmosphere to have been
observed to exhibit metal emission lines as a direct result of intense
irradiation. The equivalent widths of many of these lines show a significant
difference between the day and night sides of the brown dwarf. This is likely
an indication that efficient heat redistribution may not be happening on this
object, in agreement with models of hot Jupiter atmospheres. The H$\alpha$ line
strength variation shows a strong phase dependency as does the width. We have
simulated the Ca II emission lines using a model that includes the brown dwarf
Roche geometry and limb darkening and we estimate the mass ratio of the system
to be 0.135$\pm$0.004. We also apply a gas-phase equilibrium code using a
prescribed drift-phoenix model to examine how the chemical composition of the
brown dwarf upper atmosphere would change given an outward temperature
increase, and discuss the possibility that this would induce a chromosphere
above the brown dwarf atmosphere.
