  We present a spectral analysis of a brief Chandra/HETG observation of the
neutron star low-mass X-ray binary GX~340+0. The high-resolution spectrum
reveals evidence of ionized absorption in the Fe K band. The strongest feature,
an absorption line at approximately 6.9 keV, is required at the 5 sigma level
of confidence via an F-test. Photoionization modeling with XSTAR grids suggests
that the line is the most prominent part of a disk wind with an apparent
outflow speed of v = 0.04c. This interpretation is preferred at the 4 sigma
level over a scenario in which the line is H-like Fe XXVI at a modest
red-shift. The wind may achieve this speed owing to its relatively low
ionization, enabling driving by radiation pressure on lines; in this sense, the
wind in GX 340+0 may be the stellar-mass equivalent of the flows in broad
absorption line quasars (BALQSOs). If the gas has a unity volume filling
factor, the mass ouflow rate in the wind is over 10^-5 Msun/year, and the
kinetic power is nearly 10^39 erg/s (or, 5-6 times the radiative Eddington
limit for a neutron star). However, geometrical considerations - including a
small volume filling factor and low covering factor - likely greatly reduce
these values.
